From 1941aef393b2f072c8558f12567798d6cd7dcf89 Mon Sep 17 00:00:00 2001 From: Phil Marshall Date: Sun, 16 Sep 2018 19:09:29 -0400 Subject: [PATCH 1/6] Modified READMEs to refer to the 'COSEP' --- .gitignore | 3 + README.md | 86 +- whitepaper/README.md | 17 +- whitepaper/references.bib.backup | 4684 ------------------------------ 4 files changed, 61 insertions(+), 4729 deletions(-) delete mode 100644 whitepaper/references.bib.backup diff --git a/.gitignore b/.gitignore index 325f256..014b946 100644 --- a/.gitignore +++ b/.gitignore @@ -121,3 +121,6 @@ sympy-plots-for-*.tex/ # Other stuff: *_standalone.tex attic +review +arxiv +MAF diff --git a/README.md b/README.md index 493cfa0..7bbdd12 100644 --- a/README.md +++ b/README.md @@ -2,29 +2,39 @@ Welcome to the online community thinking about LSST survey strategy ("cadence"), with quantifications via the Metric Analysis Framework. -We are writing a white paper on this topic, primarily composed of a set of individual science cases that are either very important, and somehow stress the observing strategy, and describing how we expect them to be sensitive to LSST observing strategy. MAF metric calculations are then being designed and implemented: these form the quantitative backbone of the document. You may have heard of the coming "Cadence Wars" - this white paper represents the "Cadence Diplomacy" that will allow us, as a community, to avoid, or at least manage, that conflict. We welcome contributions from all around the LSST Science community. +Together, we are developing the LSST Community Observing Strategy Evaluation Paper (COSEP), a living document that explores the effects that changes to the LSST survey strategy would have on the detailed performance of the anticipated science investigations. - +You may have heard of the coming "Cadence Wars" - the COSEP represents the "Cadence Diplomacy" that will allow us, as a community, to avoid, or at least manage, that conflict. +As it explains in its introduction, the COSEP is "_the_ vehicle for the community to communicate to the LSST Project regarding the Wide-Fast-Deep and special survey observing strategies." +We welcome contributions from all around the LSST Science community. -* **[Read the current draft of the white paper](https://github.com/LSSTScienceCollaborations/ObservingStrategy/blob/pdf/whitepaper/LSST_Observing_Strategy_White_Paper.pdf +The first version of the COSEP was posted to the arxiv in Summer 2017, and can be downloaded [here](https://arxiv.org/abs/1708.04058v1). +It was structured as a set of individual science cases that are each very important, and/or somehow stress the observing strategy; each of these sections described how we expect them to be sensitive to LSST observing strategy, and many included a MAF metric analysis (or the design of one). These science sections formed the quantitative backbone of the document, and followed an introductory chapter that laid out the suite of LSST Project-simulated cadences that existed at the time. The v1 COSEP's primary conclusions were: + +1. The LSST Project should simulate, analyze and optimize the rolling cadence idea; +2. The LSST Project should execute a systematic effort to further improve the ultimate LSST survey strategy. + +These conclusions informed the 2018 [Call for White Papers on LSST Cadence Optimization](https://docushare.lsst.org/docushare/dsweb/Get/Document-28382), which anticipates that the performance evaluation components of the white papers solicited will also be added to the COSEP, to provide a comprehensive reference point for survey strategy evaluation. We are currently setting up the COSEP to accept the 2018 white papers, on the way to producing version 2 in April 2019. + + +* **[Read the current draft of the COSEP](https://github.com/LSSTScienceCollaborations/ObservingStrategy/blob/pdf/whitepaper/LSST_Observing_Strategy_White_Paper.pdf )** (automatically generated PDF, rebuilt every time the `master` branch is updated) [![Build Status](https://travis-ci.org/LSSTScienceCollaborations/ObservingStrategy.svg?branch=master)](https://travis-ci.org/LSSTScienceCollaborations/ObservingStrategy) -* **[Download v1.0 of the white paper](https://github.com/LSSTScienceCollaborations/ObservingStrategy/raw/master/whitepaper/releases/LSST_Observing_Strategy_White_Paper_v1.0.pdf)** This is the initial arxiv version, visible at https://arxiv.org/abs/1708.04058 +* **[Download v1.0 of the COSEP](https://github.com/LSSTScienceCollaborations/ObservingStrategy/raw/master/whitepaper/releases/LSST_Observing_Strategy_White_Paper_v1.0.pdf)** This is the initial arxiv version, visible at https://arxiv.org/abs/1708.04058v1 * **[Join the conversation about this project at its issues list](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues)** -* **[Gauge the project's activity level](https://github.com/LSSTScienceCollaborations/ObservingStrategy/pulse/halfweekly)** +* **[Gauge the project's current activity level](https://github.com/LSSTScienceCollaborations/ObservingStrategy/pulse/halfweekly)** -* **[Suggest a new `OpSim` experiment](https://github.com/LSSTScienceCollaborations/ObservingStrategy/blob/master/opsim/README.md)** +* **[Suggest a new `OpSim` experiment (a simulated cadence)](https://github.com/LSSTScienceCollaborations/ObservingStrategy/blob/master/opsim/README.md)** * **[Suggest some interesting commissioning observations](https://github.com/LSSTScienceCollaborations/ObservingStrategy/blob/master/commissioning/README.md)** #### Shortcuts -* Guidelines for how to get involved are [in the introduction of the white paper itself, in Section 1.4](https://github.com/LSSTScienceCollaborations/ObservingStrategy/blob/master/whitepaper/preface.tex) +* Guidelines for how to get involved are [in the introduction of the COSEP itself, in Section 1.4](https://github.com/LSSTScienceCollaborations/ObservingStrategy/blob/master/whitepaper/preface.tex) * For help getting started with git and GitHub, see this [handy guide](https://github.com/drphilmarshall/GettingStarted#top). * Shortened URL for this repository (for passing around): [http://ls.st/o5k](http://ls.st/o5k) * Community-contributed MAF metric code at the [`sims_maf_contrib` repository](https://github.com/LSST-nonproject/sims_maf_contrib/wiki) @@ -43,43 +53,43 @@ End of old workshop links --> ## Contacts -This effort is being coordinated by [Zeljko Ivezic](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues/new?body=@ivezic) and [Beth Willman](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues/new?body=@bethwillman), while [Phil Marshall](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues/new?body=@drphilmarshall) is the white paper's editor-in-chief. Any of them can propagate your privately-communicated concerns into a redacted issue on this repository. Contributions are very welcome from all round the LSST science collaborations, and beyond. Perhaps we are missing a science case? Or an idea for how to perturb the observing strategy? We'd like to hear from you! Please send all your feedback to [this repo's issues](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues). +This effort is being coordinated by [Phil Marshall](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues/new?body=@drphilmarshall) (the v1 COSEP's editor-in-chief), with guidance from [Zeljko Ivezic](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues/new?body=@ivezic) and [Lynne Jones](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues/new?body=@rhiannonlynne). Any of them can propagate your privately-communicated concerns into a redacted issue on this repository. Contributions are very welcome from all round the LSST science collaborations, and beyond. Perhaps we are missing a science case? Or an idea for how to perturb the observing strategy? We'd like to hear from you! Please send all your feedback to [this repo's issues](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues). -All white paper content is Copyright 2015, 2016, 2017 The Authors. If you make use of the ideas and results in the white paper in your research, please cite it as **"(LSST Science Collaborations 2017)"**, and provide the URL of this repository: https://github.com/LSSTScienceCollaborations/ObservingStrategy. The BibTeX entry for the white paper is below. Thanks! +All COSEP content is Copyright 2015, 2016, 2017, 2018 The Authors. If you make use of the ideas and results in the COSEP in your research, please cite it as **"(LSST Science Collaborations 2017)"**, and provide the URL of this repository: https://github.com/LSSTScienceCollaborations/ObservingStrategy. The BibTeX entry for the v1 COSEP is below. Thanks! ``` -@ARTICLE{LSSTObservingStrategyWhitePaper, - author = {{LSST Science Collaborations} and {Marshall}, P. and {Anguita}, T. and - {Bianco}, F.~B. and {Bellm}, E.~C. and {Brandt}, N. and {Clarkson}, W. and - {Connolly}, A. and {Gawiser}, E. and {Ivezic}, Z. and {Jones}, L. and - {Lochner}, M. and {Lund}, M.~B. and {Mahabal}, A. and {Nidever}, D. and - {Olsen}, K. and {Ridgway}, S. and {Rhodes}, J. and {Shemmer}, O. and - {Trilling}, D. and {Vivas}, K. and {Walkowicz}, L. and {Willman}, B. and - {Yoachim}, P. and {Anderson}, S. and {Antilogus}, P. and {Angus}, R. and - {Arcavi}, I. and {Awan}, H. and {Biswas}, R. and {Bell}, K.~J. and - {Bennett}, D. and {Britt}, C. and {Buzasi}, D. and {Casetti-Dinescu}, D.~I. and - {Chomiuk}, L. and {Claver}, C. and {Cook}, K. and {Davenport}, J. and - {Debattista}, V. and {Digel}, S. and {Doctor}, Z. and {Firth}, R.~E. and - {Foley}, R. and {Fong}, W.-f. and {Galbany}, L. and {Giampapa}, M. and - {Gizis}, J.~E. and {Graham}, M.~L. and {Grillmair}, C. and {Gris}, P. and - {Haiman}, Z. and {Hartigan}, P. and {Hawley}, S. and {Hlozek}, R. and - {Jha}, S.~W. and {Johns-Krull}, C. and {Kanbur}, S. and {Kalogera}, V. and - {Kashyap}, V. and {Kasliwal}, V. and {Kessler}, R. and {Kim}, A. and - {Kurczynski}, P. and {Lahav}, O. and {Liu}, M.~C. and {Malz}, A. and - {Margutti}, R. and {Matheson}, T. and {McEwen}, J.~D. and {McGehee}, P. and - {Meibom}, S. and {Meyers}, J. and {Monet}, D. and {Neilsen}, E. and - {Newman}, J. and {O'Dowd}, M. and {Peiris}, H.~V. and {Penny}, M.~T. and - {Peters}, C. and {Poleski}, R. and {Ponder}, K. and {Richards}, G. and - {Rho}, J. and {Rubin}, D. and {Schmidt}, S. and {Schuhmann}, R.~L. and - {Shporer}, A. and {Slater}, C. and {Smith}, N. and {Soares-Santos}, M. and - {Stassun}, K. and {Strader}, J. and {Strauss}, M. and {Street}, R. and - {Stubbs}, C. and {Sullivan}, M. and {Szkody}, P. and {Trimble}, V. and - {Tyson}, T. and {de Val-Borro}, M. and {Valenti}, S. and {Wagoner}, R. and +@ARTICLE{LSST-COSEP, + author = {{LSST Science Collaborations} and {Marshall}, P. and {Anguita}, T. and + {Bianco}, F.~B. and {Bellm}, E.~C. and {Brandt}, N. and {Clarkson}, W. and + {Connolly}, A. and {Gawiser}, E. and {Ivezic}, Z. and {Jones}, L. and + {Lochner}, M. and {Lund}, M.~B. and {Mahabal}, A. and {Nidever}, D. and + {Olsen}, K. and {Ridgway}, S. and {Rhodes}, J. and {Shemmer}, O. and + {Trilling}, D. and {Vivas}, K. and {Walkowicz}, L. and {Willman}, B. and + {Yoachim}, P. and {Anderson}, S. and {Antilogus}, P. and {Angus}, R. and + {Arcavi}, I. and {Awan}, H. and {Biswas}, R. and {Bell}, K.~J. and + {Bennett}, D. and {Britt}, C. and {Buzasi}, D. and {Casetti-Dinescu}, D.~I. and + {Chomiuk}, L. and {Claver}, C. and {Cook}, K. and {Davenport}, J. and + {Debattista}, V. and {Digel}, S. and {Doctor}, Z. and {Firth}, R.~E. and + {Foley}, R. and {Fong}, W.-f. and {Galbany}, L. and {Giampapa}, M. and + {Gizis}, J.~E. and {Graham}, M.~L. and {Grillmair}, C. and {Gris}, P. and + {Haiman}, Z. and {Hartigan}, P. and {Hawley}, S. and {Hlozek}, R. and + {Jha}, S.~W. and {Johns-Krull}, C. and {Kanbur}, S. and {Kalogera}, V. and + {Kashyap}, V. and {Kasliwal}, V. and {Kessler}, R. and {Kim}, A. and + {Kurczynski}, P. and {Lahav}, O. and {Liu}, M.~C. and {Malz}, A. and + {Margutti}, R. and {Matheson}, T. and {McEwen}, J.~D. and {McGehee}, P. and + {Meibom}, S. and {Meyers}, J. and {Monet}, D. and {Neilsen}, E. and + {Newman}, J. and {O'Dowd}, M. and {Peiris}, H.~V. and {Penny}, M.~T. and + {Peters}, C. and {Poleski}, R. and {Ponder}, K. and {Richards}, G. and + {Rho}, J. and {Rubin}, D. and {Schmidt}, S. and {Schuhmann}, R.~L. and + {Shporer}, A. and {Slater}, C. and {Smith}, N. and {Soares-Santos}, M. and + {Stassun}, K. and {Strader}, J. and {Strauss}, M. and {Street}, R. and + {Stubbs}, C. and {Sullivan}, M. and {Szkody}, P. and {Trimble}, V. and + {Tyson}, T. and {de Val-Borro}, M. and {Valenti}, S. and {Wagoner}, R. and {Wood-Vasey}, W.~M. and {Zauderer}, B.~A.}, title = "{Science-Driven Optimization of the LSST Observing Strategy}", journal = {ArXiv e-prints}, archivePrefix = "arXiv", - eprint = {1708.04058}, + eprint = {1708.04058v1}, primaryClass = "astro-ph.IM", keywords = {Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics}, year = 2017, diff --git a/whitepaper/README.md b/whitepaper/README.md index bb65e53..1cbd32e 100644 --- a/whitepaper/README.md +++ b/whitepaper/README.md @@ -2,23 +2,26 @@ [![Build Status](https://travis-ci.org/LSSTScienceCollaborations/ObservingStrategy.svg?branch=master)](https://travis-ci.org/LSSTScienceCollaborations/ObservingStrategy) -A community white paper about LSST observing strategy, with quantifications via the the Metric Analysis Framework. +the LSST Community Observing Strategy Evaluation Paper (COSEP) is a living document that explores the effects that changes to the LSST survey strategy would have on the detailed performance of the anticipated science investigations, +with quantifications via the the Metric Analysis Framework. -* **[Read the current version of the paper here](http://www.slac.stanford.edu/~digel/ObservingStrategy/whitepaper/LSST_Observing_Strategy_White_Paper.pdf)** (automatically generated PDF, updated hourly - [log file is here](http://www.slac.stanford.edu/~digel/ObservingStrategy/whitepaper/LSST_Observing_Strategy_White_Paper.log)) +* **[Read the current draft of the COSEP](https://github.com/LSSTScienceCollaborations/ObservingStrategy/blob/pdf/whitepaper/LSST_Observing_Strategy_White_Paper.pdf +)** (automatically generated PDF, rebuilt every time the `master` branch is updated) +[![Build Status](https://travis-ci.org/LSSTScienceCollaborations/ObservingStrategy.svg?branch=master)](https://travis-ci.org/LSSTScienceCollaborations/ObservingStrategy) ## How to contribute We welcome contributions from all members of the LSST project and science community! -The white paper contains guidelines for authors on how to get involved - including hyperlinks to useful resources. +The COSEP contains guidelines for authors on how to get involved - including hyperlinks to useful resources. -If you would like to propose changes or additions to the white paper, please: +If you would like to propose changes or additions to the COSEP, please: * 1) First, read the [paper](http://www.slac.stanford.edu/~digel/ObservingStrategy/whitepaper/LSST_Observing_Strategy_White_Paper.pdf) and the [issues](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues) to see if your suggestion is already being discussed. -* 2) Then, to edit the paper, first [fork](https://help.github.com/articles/fork-a-repo/) this repository, clone it to your local machine, and edit the text. To compile the PDF, just hit `make` in the `whitepaper` folder. +* 2) Then, to edit the COSEP, first [fork](https://help.github.com/articles/fork-a-repo/) this repository, clone it to your local machine, and edit the text. To compile the PDF, just hit `make` in the `whitepaper` folder. -* 3) After you have committed and pushed your changes, you can submit a [pull request](https://help.github.com/articles/using-pull-requests/) to get your work accepted into the white paper by the editors. Thanks! +* 3) After you have committed and pushed your changes, you can submit a [pull request](https://help.github.com/articles/using-pull-requests/) to get your work accepted into the COSEP by the editors. Thanks! If the document does not compile, and you cannot fix the problem, please submit the error message and your preliminary diagnosis as an [issue](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues). @@ -30,4 +33,4 @@ Section Leads: you will need to make sure that your section is correctly read in ## License, credit etc -This paper contains research in progress. All content is Copyright 2015, 2016, 2017 The LSST Science Collaborations. If you would like to cite it, please do so as "(LSST Science Collaborations, in preparation)" and provide a footnote containing the URL of this repository: https://github.com/LSSTScienceCollaborations/ObservingStrategy. The LaTeX and python code used here is distributed for you to use at your own risk under the MIT License. We are grateful to the developers of [yahapj.bst](https://github.com/AASJournals/yahapj) for enabling our hyper-linked reference list. +This paper contains research in progress. All content is Copyright 2015, 2016, 2017, 2018 The LSST Science Collaborations. If you would like to cite it, please do so as "(LSST Science Collaborations, in preparation)" and provide a footnote containing the URL of this repository: https://github.com/LSSTScienceCollaborations/ObservingStrategy. The LaTeX and python code used here is distributed for you to use at your own risk under the MIT License. We are grateful to the developers of [yahapj.bst](https://github.com/AASJournals/yahapj) for enabling our hyper-linked reference list. diff --git a/whitepaper/references.bib.backup b/whitepaper/references.bib.backup deleted file mode 100644 index 40b02f6..0000000 --- a/whitepaper/references.bib.backup +++ /dev/null @@ -1,4684 +0,0 @@ -@ARTICLE{Kessler2015, -author = {{Kessler}, R. and {Marriner}, J. and {Childress}, M. and {Covarrubias}, R. and - {D'Andrea}, C.~B. and {Finley}, D.~A. and {Fischer}, J. and - {Foley}, R.~J. and {Goldstein}, D. and {Gupta}, R.~R. and {Kuehn}, K. and - {Marcha}, M. and {Nichol}, R.~C. and {Papadopoulos}, A. and - {Sako}, M. and {Scolnic}, D. and {Smith}, M. and {Sullivan}, M. and - {Wester}, W. and {Yuan}, F. and {Abbott}, T. and {Abdalla}, F.~B. and - {Allam}, S. and {Benoit-L{\'e}vy}, A. and {Bernstein}, G.~M. and - {Bertin}, E. and {Brooks}, D. and {Carnero Rosell}, A. and {Carrasco Kind}, M. and - {Castander}, F.~J. and {Crocce}, M. and {da Costa}, L.~N. and - {Desai}, S. and {Diehl}, H.~T. and {Eifler}, T.~F. and {Fausti Neto}, A. and - {Flaugher}, B. and {Frieman}, J. and {Gerdes}, D.~W. and {Gruen}, D. and - {Gruendl}, R.~A. and {Honscheid}, K. and {James}, D.~J. and - {Kuropatkin}, N. and {Li}, T.~S. and {Maia}, M.~A.~G. and {Marshall}, J.~L. and - {Martini}, P. and {Miller}, C.~J. and {Miquel}, R. and {Nord}, B. and - {Ogando}, R. and {Plazas}, A.~A. and {Reil}, K. and {Romer}, A.~K. and - {Roodman}, A. and {Sanchez}, E. and {Sevilla-Noarbe}, I. and - {Smith}, R.~C. and {Soares-Santos}, M. and {Sobreira}, F. and - {Tarle}, G. and {Thaler}, J. and {Thomas}, R.~C. and {Tucker}, D. and - {Walker}, A.~R. and {DES Collaboration}}, - title = "{The Difference Imaging Pipeline for the Transient Search in the Dark Energy Survey}", - journal = {\aj}, -archivePrefix = "arXiv", - eprint = {1507.05137}, - primaryClass = "astro-ph.IM", - keywords = {supernovae: general, techniques: image processing}, - year = 2015, - month = dec, - volume = 150, - eid = {172}, - pages = {172}, - doi = {10.1088/0004-6256/150/6/172}, - adsurl = {http://adsabs.harvard.edu/abs/2015AJ....150..172K}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - - - -@ARTICLE{Frieman2008, - author = {{Frieman}, J.~A. and {Turner}, M.~S. and {Huterer}, D.}, - title = "{Dark Energy and the Accelerating Universe}", - journal = {\araa}, -archivePrefix = "arXiv", - eprint = {0803.0982}, - year = 2008, - month = sep, - volume = 46, - pages = {385-432}, - doi = {10.1146/annurev.astro.46.060407.145243}, - adsurl = {http://adsabs.harvard.edu/abs/2008ARA%26A..46..385F}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Riess1998, - author = {{Riess}, A.~G. and {Filippenko}, A.~V. and {Challis}, P. and - {Clocchiatti}, A. and {Diercks}, A. and {Garnavich}, P.~M. and - {Gilliland}, R.~L. and {Hogan}, C.~J. and {Jha}, S. and {Kirshner}, R.~P. and - {Leibundgut}, B. and {Phillips}, M.~M. and {Reiss}, D. and {Schmidt}, B.~P. and - {Schommer}, R.~A. and {Smith}, R.~C. and {Spyromilio}, J. and - {Stubbs}, C. and {Suntzeff}, N.~B. and {Tonry}, J.}, - title = "{Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant}", - journal = {\aj}, - eprint = {astro-ph/9805201}, - keywords = {COSMOLOGY: OBSERVATIONS, STARS: SUPERNOVAE: GENERAL}, - year = 1998, - month = sep, - volume = 116, - pages = {1009-1038}, - doi = {10.1086/300499}, - adsurl = {http://adsabs.harvard.edu/abs/1998AJ....116.1009R}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Suzuki2012, - author = {{Suzuki}, N. and {Rubin}, D. and {Lidman}, C. and {Aldering}, G. and - {Amanullah}, R. and {Barbary}, K. and {Barrientos}, L.~F. and - {Botyanszki}, J. and {Brodwin}, M. and {Connolly}, N. and {Dawson}, K.~S. and - {Dey}, A. and {Doi}, M. and {Donahue}, M. and {Deustua}, S. and - {Eisenhardt}, P. and {Ellingson}, E. and {Faccioli}, L. and - {Fadeyev}, V. and {Fakhouri}, H.~K. and {Fruchter}, A.~S. and - {Gilbank}, D.~G. and {Gladders}, M.~D. and {Goldhaber}, G. and - {Gonzalez}, A.~H. and {Goobar}, A. and {Gude}, A. and {Hattori}, T. and - {Hoekstra}, H. and {Hsiao}, E. and {Huang}, X. and {Ihara}, Y. and - {Jee}, M.~J. and {Johnston}, D. and {Kashikawa}, N. and {Koester}, B. and - {Konishi}, K. and {Kowalski}, M. and {Linder}, E.~V. and {Lubin}, L. and - {Melbourne}, J. and {Meyers}, J. and {Morokuma}, T. and {Munshi}, F. and - {Mullis}, C. and {Oda}, T. and {Panagia}, N. and {Perlmutter}, S. and - {Postman}, M. and {Pritchard}, T. and {Rhodes}, J. and {Ripoche}, P. and - {Rosati}, P. and {Schlegel}, D.~J. and {Spadafora}, A. and {Stanford}, S.~A. and - {Stanishev}, V. and {Stern}, D. and {Strovink}, M. and {Takanashi}, N. and - {Tokita}, K. and {Wagner}, M. and {Wang}, L. and {Yasuda}, N. and - {Yee}, H.~K.~C. and {Supernova Cosmology Project}, T.}, - title = "{The Hubble Space Telescope Cluster Supernova Survey. 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primaryClass = "astro-ph.SR", - keywords = {supernovae: general, supernovae: individual: SN 2009jf, galaxies: individual: NGC 7479}, - year = 2011, - month = oct, - volume = 416, - pages = {3138-3159}, - doi = {10.1111/j.1365-2966.2011.19262.x}, - adsurl = {http://adsabs.harvard.edu/abs/2011MNRAS.416.3138V}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Rubin16, - author = {{Rubin}, A. and {Gal-Yam}, A. and {De Cia}, A. and {Horesh}, A. and - {Khazov}, D. and {Ofek}, E.~O. and {Kulkarni}, S.~R. and {Arcavi}, I. and - {Manulis}, I. and {Yaron}, O. and {Vreeswijk}, P. and {Kasliwal}, M.~M. and - {Ben-Ami}, S. and {Perley}, D.~A. and {Cao}, Y. and {Cenko}, S.~B. and - {Rebbapragada}, U.~D. and {Wo{\'z}niak}, P.~R. and {Filippenko}, A.~V. and - {Clubb}, K.~I. and {Nugent}, P.~E. and {Pan}, Y.-C. and {Badenes}, C. and - {Howell}, D.~A. and {Valenti}, S. and {Sand}, D. and {Sollerman}, J. and - {Johansson}, J. and {Leonard}, D.~C. and {Horst}, J.~C. and - {Armen}, S.~F. and {Fedrow}, J.~M. and {Quimby}, R.~M. and {Mazzali}, P. and - {Pian}, E. and {Sternberg}, A. and {Matheson}, T. and {Sullivan}, M. and - {Maguire}, K. and {Lazarevic}, S.}, - title = "{Type II Supernova Energetics and Comparison of Light Curves to Shock-cooling Models}", - journal = {\apj}, -archivePrefix = "arXiv", - eprint = {1512.00733}, - primaryClass = "astro-ph.HE", - keywords = {supernovae: general}, - year = 2016, - month = mar, - volume = 820, - eid = {33}, - pages = {33}, - doi = {10.3847/0004-637X/820/1/33}, - adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...820...33R}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Abbott2016LRR, - author = {{Abbott}, B.~P. and {Abbott}, R. and {Abbott}, T.~D. and {Abernathy}, M.~R. and - {Acernese}, F. and {Ackley}, K. and {Adams}, C. and {Adams}, T. and - {Addesso}, P. and {Adhikari}, R.~X. and et al.}, - title = "{Prospects for Observing and Localizing Gravitational-Wave Transients with Advanced LIGO and Advanced Virgo}", - journal = {Living Reviews in Relativity}, -archivePrefix = "arXiv", - eprint = {1304.0670}, - primaryClass = "gr-qc", - keywords = {Data analysis, Gravitational-wave detectors, Gravitational waves, Electromagnetic counterparts}, - year = 2016, - month = feb, - volume = 19, - doi = {10.1007/lrr-2016-1}, - adsurl = {http://adsabs.harvard.edu/abs/2016LRR....19....1A}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Bianco11, - author = {{Bianco}, F.~B. and {Howell}, D.~A. and {Sullivan}, M. and {Conley}, A. and - {Kasen}, D. and {Gonz{\'a}lez-Gait{\'a}n}, S. and {Guy}, J. and - {Astier}, P. and {Balland}, C. and {Carlberg}, R.~G. and {Fouchez}, D. and - {Fourmanoit}, N. and {Hardin}, D. and {Hook}, I. and {Lidman}, C. and - {Pain}, R. and {Palanque-Delabrouille}, N. and {Perlmutter}, S. and - {Perrett}, K.~M. and {Pritchet}, C.~J. and {Regnault}, N. and - {Rich}, J. and {Ruhlmann-Kleider}, V.}, - title = "{Constraining Type Ia Supernovae Progenitors from Three Years of Supernova Legacy Survey Data}", - journal = {\apj}, -archivePrefix = "arXiv", - eprint = {1106.4008}, - primaryClass = "astro-ph.CO", - keywords = {methods: data analysis, supernovae: general, white dwarfs}, - year = 2011, - month = nov, - volume = 741, - eid = {20}, - pages = {20}, - doi = {10.1088/0004-637X/741/1/20}, - adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...741...20B}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Olling15, - author = {{Olling}, R.~P. and {Mushotzky}, R. and {Shaya}, E.~J. and {Rest}, A. and - {Garnavich}, P.~M. and {Tucker}, B.~E. and {Kasen}, D. and {Margheim}, S. and - {Filippenko}, A.~V.}, - title = "{No signature of ejecta interaction with a stellar companion in three type Ia supernovae}", - journal = {\nat}, - year = 2015, - month = may, - volume = 521, - pages = {332-335}, - doi = {10.1038/nature14455}, - adsurl = {http://adsabs.harvard.edu/abs/2015Natur.521..332O}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} -@ARTICLE{Li11b, - author = {{Li}, W. and {Leaman}, J. and {Chornock}, R. and {Filippenko}, A.~V. and - {Poznanski}, D. and {Ganeshalingam}, M. and {Wang}, X. and {Modjaz}, M. and - {Jha}, S. and {Foley}, R.~J. and {Smith}, N.}, - title = "{Nearby supernova rates from the Lick Observatory Supernova Search - II. The observed luminosity functions and fractions of supernovae in a complete sample}", - journal = {\mnras}, -archivePrefix = "arXiv", - eprint = {1006.4612}, - primaryClass = "astro-ph.SR", - keywords = {supernovae: general}, - year = 2011, - month = apr, - volume = 412, - pages = {1441-1472}, - doi = {10.1111/j.1365-2966.2011.18160.x}, - adsurl = {http://adsabs.harvard.edu/abs/2011MNRAS.412.1441L}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Li11, - author = {{Li}, W. and {Bloom}, J.~S. and {Podsiadlowski}, P. and {Miller}, A.~A. and - {Cenko}, S.~B. and {Jha}, S.~W. and {Sullivan}, M. and {Howell}, D.~A. and - {Nugent}, P.~E. and {Butler}, N.~R. and {Ofek}, E.~O. and {Kasliwal}, M.~M. and - {Richards}, J.~W. and {Stockton}, A. and {Shih}, H.-Y. and {Bildsten}, L. and - {Shara}, M.~M. and {Bibby}, J. and {Filippenko}, A.~V. and {Ganeshalingam}, M. and - {Silverman}, J.~M. and {Kulkarni}, S.~R. and {Law}, N.~M. and - {Poznanski}, D. and {Quimby}, R.~M. and {McCully}, C. and {Patel}, B. and - {Maguire}, K. and {Shen}, K.~J.}, - title = "{Exclusion of a luminous red giant as a companion star to the progenitor of supernova SN 2011fe}", - journal = {\nat}, -archivePrefix = "arXiv", - eprint = {1109.1593}, - primaryClass = "astro-ph.CO", - year = 2011, - month = dec, - volume = 480, - pages = {348-350}, - doi = {10.1038/nature10646}, - adsurl = {http://adsabs.harvard.edu/abs/2011Natur.480..348L}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Dilday12, - author = {{Dilday}, B. and {Howell}, D.~A. and {Cenko}, S.~B. and {Silverman}, J.~M. and - {Nugent}, P.~E. and {Sullivan}, M. and {Ben-Ami}, S. and {Bildsten}, L. and - {Bolte}, M. and {Endl}, M. and {Filippenko}, A.~V. and {Gnat}, O. and - {Horesh}, A. and {Hsiao}, E. and {Kasliwal}, M.~M. and {Kirkman}, D. and - {Maguire}, K. and {Marcy}, G.~W. and {Moore}, K. and {Pan}, Y. and - {Parrent}, J.~T. and {Podsiadlowski}, P. and {Quimby}, R.~M. and - {Sternberg}, A. and {Suzuki}, N. and {Tytler}, D.~R. and {Xu}, D. and - {Bloom}, J.~S. and {Gal-Yam}, A. and {Hook}, I.~M. and {Kulkarni}, S.~R. and - {Law}, N.~M. and {Ofek}, E.~O. and {Polishook}, D. and {Poznanski}, D. - }, - title = "{PTF 11kx: A Type Ia Supernova with a Symbiotic Nova Progenitor}", - journal = {Science}, -archivePrefix = "arXiv", - eprint = {1207.1306}, - year = 2012, - month = aug, - volume = 337, - pages = {942}, - doi = {10.1126/science.1219164}, - adsurl = {http://adsabs.harvard.edu/abs/2012Sci...337..942D}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Nugent02, - author = {{Nugent}, P. and {Kim}, A. and {Perlmutter}, S.}, - title = "{K-Corrections and Extinction Corrections for Type Ia Supernovae}", - journal = {\pasp}, - eprint = {astro-ph/0205351}, - keywords = {Cosmology: Observations, Stars: Supernovae: General}, - year = 2002, - month = aug, - volume = 114, - pages = {803-819}, - doi = {10.1086/341707}, - adsurl = {http://adsabs.harvard.edu/abs/2002PASP..114..803N}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@ARTICLE{Kasen10, - author = {{Kasen}, D.}, - title = "{Seeing the Collision of a Supernova with Its Companion Star}", - journal = {\apj}, -archivePrefix = "arXiv", - eprint = {0909.0275}, - primaryClass = "astro-ph.HE", - keywords = {binaries: general, supernovae: general, X-rays: bursts}, - year = 2010, - month = jan, - volume = 708, - pages = {1025-1031}, - doi = {10.1088/0004-637X/708/2/1025}, - adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...708.1025K}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@article{Arcavi2014, -abstract = {We present the results of a Palomar Transient Factory (PTF) archival search for blue transients which lie in the magnitude range between "normal" core-collapse and superluminous supernovae (i.e. with {\$}-21\backslash,{\{}\backslashleq{\}}M{\_}{\{}R\backslash,(peak){\}}\backslash,{\{}\backslashleq{\}}-19{\$}). Of the six events found after excluding all interacting Type{\~{}}IIn and Ia-CSM supernovae, three (PTF09ge, 09axc and 09djl) are coincident with the centers of their hosts, one (10iam) is offset from the center, and for two (10nuj and 11glr) a precise offset can not be determined. All the central events have similar rise times to the He-rich tidal disruption candidate PS1-10jh, and the event with the best-sampled light curve also has similar colors and power-law decay. Spectroscopically, PTF09ge is He-rich, while PTF09axc and 09djl display broad hydrogen features around peak magnitude. All three central events are in low star-formation hosts, two of which are E+A galaxies. Our spectrum of the host of PS1-10jh displays similar properties. PTF10iam, the one offset event, is different photometrically and spectroscopically from the central events and its host displays a higher star formation rate. Finding no obvious evidence for ongoing galactic nuclei activity or recent star formation, we conclude that the three central transients likely arise from the tidal disruption of a star by a super-massive black hole. We compare the spectra of these events to tidal disruption candidates from the literature and find that all of these objects can be unified on a continuous scale of spectral properties. The accumulated evidence of this expanded sample strongly supports a tidal disruption origin for this class of nuclear transients.}, -author = {Arcavi, Iair and Gal-Yam, Avishay and Sullivan, Mark and Pan, Yen-Chen and Cenko, S. Bradley and Horesh, Assaf and Ofek, Eran O. and {De Cia}, Annalisa and Yan, Lin and Yang, Chen-Wei and Howell, D. A. and Tal, David and Kulkarni, Shrinivas R. and Tendulkar, Shriharsh P. and Tang, Sumin and Xu, Dong and Sternberg, Assaf and Cohen, Judith G. and Bloom, Joshua S. and Nugent, Peter E. and Kasliwal, Mansi M. and Perley, Daniel A. and Quimby, Robert M. and Miller, Adam A. and Theissen, Christopher A. and Laher, Russ R.}, -journal = {The Astrophysical Journal}, -keywords = {accretion,accretion disks,galaxies: nuclei,quasars: supermassive black holes}, -number = {1}, -pages = {38}, -title = {{A CONTINUUM OF H- TO He-RICH TIDAL DISRUPTION CANDIDATES WITH A PREFERENCE FOR E+A GALAXIES}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...793...38A}, -volume = {793}, -year = {2014} -} - -@article{Evans1989, -abstract = {Results are reported from a three-dimensional numerical calculation of the tidal disruption of a low-mass main-sequence star on a parabolic orbit around a massive black hole (Mh = 10 to the 6th stellar mass). The postdisruption evolution is followed until hydrodynamic forces becomes negligible and the liberated gas becomes ballistic. Also given is the rate at which bound mass returns to pericenter after orbiting the hole once. The processes that determine the time scale to circularize the debris orbits and allow an accretion torus to form are discussed. This time scale and the time scales for radiative cooling and accretion inflow determine the onset and duration of the subsequent flare in the AGN luminosity.}, -author = {Evans, Charles R. and Kochanek, Christopher S.}, -doi = {10.1086/185567}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Active Galactic Nuclei,Black Holes (Astronomy),Computational Astrophysics,Galactic Clusters,Hydrodynamic Equations,Main Sequence Stars,Stellar Luminosity,Stellar Mass}, -month = {nov}, -pages = {L13}, -title = {{The tidal disruption of a star by a massive black hole}}, -url = {http://adsabs.harvard.edu/abs/1989ApJ...346L..13E}, -volume = {346}, -year = {1989} -} - -@article{French2016, -abstract = {Tidal Disruption Events (TDEs) are transient events observed when a star passes close enough to a supermassive black hole to be tidally destroyed. Many TDE candidates have been discovered in host galaxies whose spectra have weak or no line emission yet strong Balmer line absorption, indicating a period of intense star formation that has recently ended. As such, TDE host galaxies fall into the rare class of quiescent Balmer-strong galaxies. Here, we quantify the fraction of galaxies in the Sloan Digital Sky Survey (SDSS) with spectral properties like those of TDE hosts, determining the extent to which TDEs are over-represented in such galaxies. Galaxies whose spectra have Balmer absorption {\{}{\{}H{\}}{\}}{\{}$\delta$ {\}}{\{}{\{}A{\}}{\}} - $\sigma$(H{\{}$\delta$ {\}}{\{}{\{}A{\}}{\}}) {\textgreater} 4 {\AA} (where $\sigma$(H{\{}$\delta$ {\}}{\{}{\{}A{\}}{\}}) is the error in the Lick {\{}{\{}H{\}}{\}}{\{}$\delta$ {\}}{\{}{\{}A{\}}{\}} index) and H$\alpha$ emission equivalent width (EW) {\textless} 3 {\AA} have had a strong starburst in the last ˜Gyr. They represent 0.2{\%} of the local galaxy population, yet host 3 of 8 (37.5{\%}) optical/UV-selected TDE candidates. A broader cut, {\{}{\{}H{\}}{\}}{\{}$\delta$ {\}}{\{}{\{}A{\}}{\}}$\backslash$quad $\backslash$gt 1.31 {\AA} and H$\alpha$ EW {\textless} 3 {\AA}, nets only 2.3{\%} of SDSS galaxies, but 6 of 8 (75{\%}) optical/UV TDE hosts. Thus, quiescent Balmer-strong galaxies are over-represented among the TDE hosts by a factor of 33-190. The high-energy-selected TDE Swift J1644 also lies in a galaxy with strong Balmer lines and weak H$\alpha$ emission, implying a $\backslash$gt 80× enhancement in such hosts and providing an observational link between the $\gamma$/X-ray-bright and optical/UV-bright TDE classes.}, -author = {French, K. Decker and Arcavi, Iair and Zabludoff, Ann}, -doi = {10.3847/2041-8205/818/1/L21}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: nuclei}, -month = {feb}, -number = {1}, -pages = {L21}, -title = {{TIDAL DISRUPTION EVENTS PREFER UNUSUAL HOST GALAXIES}}, -url = {http://adsabs.harvard.edu/abs/2016ApJ...818L..21F}, -volume = {818}, -year = {2016} -} - -@article{Zabludoff1996, -abstract = {The spectrum of an "E + A" galaxy (Dressier {\&} Gunn) which is dominated by a young stellar component but lacks the emission lines characteristic of any significant, on-going star formation suggests that the galaxy experienced a brief, powerful starburst within the last gigayear (Dressler {\&} Gunn; Couch {\&} Sharples). In past work, this violent star formation history and the detection of these galaxies almost exclusively in distant clusters linked them to the Butcher-Oemler (B-O) effect (Butcher {\&} Oemler) and argued for the influence of cluster environment in the evolution of galaxies. However, no statistical survey of the environments of "E+A"s had ever been made. From 11,113 galaxy spectra in the Las Campanas Redshift Survey (Shectman and coworkers), we have obtained a unique and well-defined sample of 21 nearby "E+A" galaxies with the same spectral characteristics as "E+A"s in distant clusters. These "E+A"s are selected to have the strongest Balmer absorption lines (the average of the equivalent widths of H$\beta$, $\gamma$, $\delta$ is {\textgreater}5.5 A) and weakest [O II] emission-line equivalent widths ({\textless}2.5 A, which corresponds to a detection of [O II] of less than 2 $\sigma$ significance) of any of the galaxies in the survey. In contrast to inferences drawn from previous studies, we find that a large fraction (75{\%}) of nearby "E + A "s lie in the field, well outside of clusters and rich groups of galaxies. We conclude that interactions with the cluster environment, in the form of the intracluster medium or cluster potential, are not essential for "E+A" formation and therefore that the presence of these galaxies in distant clusters does not provide strong evidence for the effects of cluster environment on galaxy evolution. If one mechanism is responsible for "E+A" formation, then the observations that "E+A"s exist in the field and that at least five of the 21 in our sample have clear tidal features argue that galaxy-galaxy interactions and mergers are that mechanism. The most likely environments for such mergers are poor groups of galaxies, which have lower velocity dispersions than clusters and higher galaxy densities than the field. Groups are correlated With rich clusters and, in hierarchical models, fall into clusters in greater numbers at intermediate redshifts than they do today (cf. Bower; Lacey {\&} Cole; Kauffmann). When combined with the strong evolution observed in the field population (cf. Broadhurst and coworkers; Lilly and coworkers), our work suggests that the B-O effect may reflect the typical evolution of galaxies in groups and in the field, rather than the influence of clusters on the star formation history of galaxies.}, -author = {Zabludoff, Ann I. and Zaritsky, Dennis and Lin, Huan and Tucker, Douglas and Hashimoto, Yasuhiro and Shectman, Stephen A. and Oemler, Augustus and Kirshner, Robert P.}, -doi = {10.1086/177495}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {GALAXIES: CLUSTERS: GENERAL,GALAXIES: EVOLUTION,GALAXIES: INTERACTIONS,GALAXIES: STELLAR CONTENT}, -month = {jul}, -pages = {104}, -title = {{The Environment of ``E+A'' Galaxies}}, -url = {http://adsabs.harvard.edu/abs/1996ApJ...466..104Z}, -volume = {466}, -year = {1996} -} - -@article{Phinney1989, -author = {Phinney, E. S.}, -journal = {The Center of the Galaxy: Proceedings of the 136th Symposium of the International Astronomical Union}, -title = {{Manifestations of a Massive Black Hole in the Galactic Center}}, -url = {http://adsabs.harvard.edu/abs/1989IAUS..136..543P}, -year = {1989} -} - -@article{Dressler1983, -abstract = {The authors present 20 new spectra of objects in the field of the cluster of galaxies 3C 295 obtained with a new multislit technique. Together with previous data for this cluster, they now have good-quality spectra of 26 objects and redshifts of 23 of these. The field is heavily contaminated by a foreground cluster of galaxies. Less than half of the blue galaxies cataloged by Butcher and Oemler in this cluster are actually cluster members. The color distribution in the cluster is not unusual when compared with nearby clusters of similar morphological type. On the other hand, the six blue objects that are members of 3C 295 are all very unusual for present-day clusters, including three galaxies with active nuclei and three galaxies which have evidence for large bursts of star formation. If these data are representative, they indicate a strong evolution for these types of systems over the last 5×109 years.}, -author = {Dressler, A. and Gunn, J. E.}, -doi = {10.1086/161093}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Active Galaxies,Astronomical Spectroscopy,Balmer Series,Color,Data Acquisition,Data Reduction,Galactic Clusters,Galactic Nuclei,Red Shift,Seyfert Galaxies,Spiral Galaxies,Stellar Evolution}, -month = {jul}, -pages = {7}, -title = {{Spectroscopy of galaxies in distant clusters. II - The population of the 3C 295 cluster}}, -url = {http://adsabs.harvard.edu/abs/1983ApJ...270....7D}, -volume = {270}, -year = {1983} -} - -@article{Bono2000, -abstract = {We present a comprehensive theoretical investigation of the evolutionary properties of intermediate-mass stars. The evolutionary sequences were computed from the zero-age main sequence up to the central He exhaustion and often up to the phases that precede the carbon ignition or to the reignition of the H-shell, which marks the beginning of the thermal pulse phase. The evolutionary tracks were constructed by adopting a wide range of stellar masses (3<=M/Msolar <=15) and chemical compositions. In order to account for current uncertainties on the He to heavy elements enrichment ratio (?Y/?Z), the stellar models were computed by adopting at Z=0.02 two different He contents (Y=0.27, 0.289) and at Z=0.04 three different He contents (Y=0.29, 0.34, and 0.37). Moreover, to supply a homogeneous evolutionary scenario that accounts for young Magellanic stellar systems the calculations were also extended toward lower metallicities (Z=0.004, Z=0.01), by adopting different initial He abundances. We evaluated for both solar (Z=0.02) and super-metal-rich (SMR, Z=0.04) models the transition mass Mup between the stellar structures igniting carbon and those that develop a full electron degeneracy inside the carbon-oxygen core. We found that Mup is of the order of 7.7+/-0.5 Msolar for solar composition, while for SMR structures an increase in the He content causes a decrease in Mup, and indeed it changes from 9.5+/-0.5 Msolar at Y=0.29, to 8.7+/-0.2 Msolar at Y=0.34, and to 7.7+/-0.2 Msolar at Y=0.37. We also show that Mup presents a nonlinear behavior with metallicity, and indeed it decreases when moving from Z=0.04 to Z~0.001 and increases at lower metal contents. This finding confirms the predictions by Cassisi & Castellani and more recently by Umeda et al. and suggests that the rate of SNe type Ia depends on the chemical composition of the parent stellar population. This approach allows us to investigate in detail the evolutionary properties of classical Cepheids. In particular, we find that the range of stellar masses that perform the blue loop during the central He-burning phase narrows when moving toward metal-rich and SMR structures. This evidence and the substantial decrease in the evolutionary time spent by these structures inside the instability strip bring out that the probability of detecting long-period Cepheids in SMR stellar systems is substantially smaller than in more metal-poor systems. Moreover, and even more important, we find that the time spent by Cepheids along the subsequent crossings of the instability strip also depends on the stellar mass. In fact, our models suggest that low-mass, metal-poor Cepheids spend a substantial portion of their lifetime along the blueward excursion of the blue loop, while at higher masses (M/Msolar>=8) the time spent along the redward excursion becomes longer. Models at solar chemical composition present an opposite behavior, i.e., the time spent along the redward excursion is longer than the blueward excursion among low-mass Cepheids and vice versa for high-mass Cepheids. Oddly enough, the time spent along the blueward excursion is for models at Z=0.01 longer than the redward excursion over the entire mass range. This suggests a nonlinear dependence of crossing times on metallicity. The time spent along the first crossing of the instability strip is generally negligible with the exception of high-mass, metal-poor stellar structures for which it becomes of the order of 15\%-20\% of the total crossing time. }, -author = {Bono, G and Caputo, F and Cassisi, S and Marconi, M and Piersanti, L.and Tornambe, N}, -doi = {10.1086/317156}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {nov}, -pages = {955-971}, -title = {{Intermediate-Mass Star Models with Different Helium and Metal Contents}}, -url = {http://adsabs.harvard.edu/abs/2000ApJ...543..955B}, -volume = {543}, -year = {2000} -} - -@article{Burrows2011, -abstract = {Supermassive black holes have powerful gravitational fields with strong gradients that can destroy stars that get too close, producing a bright flare in ultraviolet and X-ray spectral regions from stellar debris that forms an accretion disk around the black hole. The aftermath of this process may have been seen several times over the past two decades in the form of sparsely sampled, slowly fading emission from distant galaxies, but the onset of the stellar disruption event has not hitherto been observed. Here we report observations of a bright X-ray flare from the extragalactic transient Swift J164449.3+573451. This source increased in brightness in the X-ray band by a factor of at least 10,000 since 1990 and by a factor of at least 100 since early 2010. We conclude that we have captured the onset of relativistic jet activity from a supermassive black hole. A companion paper comes to similar conclusions on the basis of radio observations. This event is probably due to the tidal disruption of a star falling into a supermassive black hole, but the detailed behaviour differs from current theoretical models of such events.}, -author = {Burrows, D N and Kennea, J A and Ghisellini, G and Mangano, V and Zhang, B and Page, K L and Eracleous, M and Romano, P and Sakamoto, T and Falcone, A D and Osborne, J P and Campana, S and Beardmore, A P and Breeveld, A A and Chester, M M and Corbet, R and Covino, S and Cummings, J R and D'Avanzo, P and D'Elia, V and Esposito, P and Evans, P A and Fugazza, D and Gelbord, J M and Hiroi, K and Holland, S T and Huang, K Y and Im, M and Israel, G and Jeon, Y and Jeon, Y-B and Jun, H D and Kawai, N and Kim, J H and Krimm, H A and Marshall, F E and {P M{\'{e}}sz{\'{a}}ros} and Negoro, H and Omodei, N and Park, W-K and Perkins, J S and Sugizaki, M and Sung, H-I and Tagliaferri, G and Troja, E and Ueda, Y and Urata, Y and Usui, R and Antonelli, L A and Barthelmy, S D and Cusumano, G and Giommi, P and Melandri, A and Perri, M and Racusin, J L and Sbarufatti, B and Siegel, M H and Gehrels, N}, -doi = {10.1038/nature10374}, -issn = {1476-4687}, -journal = {Nature}, -month = {aug}, -number = {7361}, -pages = {421--4}, -pmid = {21866154}, -title = {{Relativistic jet activity from the tidal disruption of a star by a massive black hole.}}, -url = {http://adsabs.harvard.edu/abs/2011Natur.476..421B}, -volume = {476}, -year = {2011} -} - -@article{Bonnerot2015, -abstract = {The potential of tidal disruption of stars to probe otherwise quiescent supermassive black holes cannot be exploited, if their dynamics is not fully understood. So far, the observational appearance of these events has been derived from analytical extrapolations of the debris dynamical properties just after disruption. By means of hydrodynamical simulations, we investigate the subsequent fallback of the stream of debris towards the black hole for stars already bound to the black hole on eccentric orbits. We demonstrate that the debris circularize due to relativistic apsidal precession which causes the stream to self-cross. The circularization time-scale varies between 1 and 10 times the period of the star, being shorter for more eccentric and/or deeper encounters. This self-crossing leads to the formation of shocks that increase the thermal energy of the debris. If this thermal energy is efficiently radiated away, the debris settle in a narrow ring at the circularization radius with shock-induced luminosities of ˜10-103 LEdd. If instead cooling is impeded, the debris form an extended torus located between the circularization radius and the semi-major axis of the star with heating rates ˜1-102 LEdd. Extrapolating our results to parabolic orbits, we infer that circularization would occur via the same mechanism in ˜1 period of the most bound debris for deeply penetrating encounters to ˜10 for grazing ones. We also anticipate the same effect of the cooling efficiency on the structure of the disc with associated luminosities of ˜1-10 LEdd and heating rates of ˜0.1-1 LEdd. In the latter case of inefficient cooling, we deduce a viscous time-scale generally shorter than the circularization time-scale. This suggests an accretion rate through the disc tracing the fallback rate, if viscosity starts acting promptly.}, -author = {Bonnerot, Cl{\'{e}}ment and Rossi, Elena M. and Lodato, Giuseppe and Price, Daniel J.}, -doi = {10.1093/mnras/stv2411}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {accretion,accretion discs,black hole physics,galaxies: nuclei,hydrodynamics}, -month = {nov}, -number = {2}, -pages = {2253--2266}, -title = {{Disc formation from tidal disruptions of stars on eccentric orbits by Schwarzschild black holes}}, -url = {http://adsabs.harvard.edu/abs/2016MNRAS.455.2253B}, -volume = {455}, -year = {2015} -} - -@article{Holoien2016, -abstract = {We present ground-based and Swift photometric and spectroscopic observations of the tidal disruption event (TDE) ASASSN-15oi, discovered at the center of 2MASX J20390918-3045201 ({\$}d\backslashsimeq216{\$} Mpc) by the All-Sky Automated Survey for SuperNovae (ASAS-SN). The source peaked at a bolometric luminosity of {\$}L\backslashsimeq1.9\backslashtimes10{\^{}}{\{}44{\}}{\$} ergs s{\$}{\^{}}{\{}-1{\}}{\$} and radiated a total energy of {\$}E\backslashsimeq5.0\backslashtimes10{\^{}}{\{}50{\}}{\$} ergs over the {\$}\backslashsim3.5{\$} months of observations. The early optical/UV emission of the source can be fit by a blackbody with temperature increasing from {\$}T\backslashsim2\backslashtimes10{\^{}}4{\$} K to {\$}T\backslashsim6\backslashtimes10{\^{}}4{\$} K while the luminosity declines from {\$}L\backslashsimeq1.9\backslashtimes10{\^{}}{\{}44{\}}{\$} ergs s{\$}{\^{}}{\{}-1{\}}{\$} to {\$}L\backslashsimeq2.8\backslashtimes10{\^{}}{\{}43{\}}{\$} ergs s{\$}{\^{}}{\{}-1{\}}{\$}, requiring the photosphere to be shrinking rapidly. The optical/UV luminosity decline is broadly consistent with an exponential decline, {\$}L\backslashpropto e{\^{}}{\{}-t/t{\_}0{\}}{\$}, with {\$}t{\_}0\backslashsimeq35{\$} days. ASASSN-15oi also exhibits roughly constant soft X-ray emission that is significantly weaker than the optical/UV emission. Spectra of the source show broad helium emission lines and strong blue continuum emission in early epochs, although these features fade rapidly and are not present {\$}\backslashsim3{\$} months after discovery. The early spectroscopic features and color evolution of ASASSN-15oi are consistent with a TDE, but the rapid spectral evolution is unique among optically-selected TDEs.}, -author = {Holoien, T. W.-S. and Kochanek, C. S. and Prieto, J. L. and Grupe, D. and Chen, Ping and Godoy-Rivera, D. and Stanek, K. Z. and Shappee, B. J. and Dong, Subo and Brown, J. S. and Basu, U. and Beacom, J. F. and Bersier, D. and Brimacombe, J. and Carlson, E. K. and Falco, E. and Johnston, E. and Madore, B. F. and Pojmanski, G. and Seibert, M.}, -journal = {eprint arXiv:1602.01088}, -keywords = {Astrophysics - High Energy Astrophysical Phenomena}, -title = {{ASASSN-15oi: A Rapidly Evolving, Luminous Tidal Disruption Event at 216 Mpc}}, -url = {http://adsabs.harvard.edu/abs/2016arXiv160201088H}, -year = {2016} -} - -@article{Donley2002, -abstract = {In recent years, luminous X-ray outbursts with variability amplitudes as high as {\~{}}400 have been serendipitously detected from a small number of active and inactive galaxies. These outbursts may result from the tidal disruptions of stars by supermassive black holes, as well as accretion disk instabilities. In order to place the first reliable constraints on the rate of such outbursts in the universe and to test the stellar tidal disruption hypothesis, we have performed a systematic and complete survey for them by cross-correlating ROSAT All-Sky Survey (RASS) and pointed Position Sensitive Proportional Counter data. We have detected five galaxies that were in outburst during the RASS, three of which show no signs of nuclear activity; these objects had been reported on individually in previous studies. After making reasonable corrections for the complicated selection effects, we conclude that the rate of large-amplitude X-ray outbursts from inactive galaxies in the local universe is {\~{}}9.1×10-6 galaxy-1 yr-1. This rate is consistent with the predicted rate of stellar tidal disruption events in such galaxies. When only the two active galaxies are considered, we find a rate for active galaxies of {\~{}}8.5×10-4 galaxy-1 yr-1. In order to place tighter constraints on these rates, additional outbursts must be detected.}, -author = {Donley, J. L. and Brandt, W. N. and Eracleous, Michael and Boller, Th.}, -doi = {10.1086/342280}, -issn = {00046256}, -journal = {The Astronomical Journal}, -keywords = {Galaxies: Active,Galaxies: Nuclei,X-Rays}, -month = {sep}, -number = {3}, -pages = {1308--1321}, -title = {{Large-Amplitude X-Ray Outbursts from Galactic Nuclei: A Systematic Survey using [ITAL]ROSAT[/ITAL] Archival Data}}, -url = {http://adsabs.harvard.edu/abs/2002AJ....124.1308D}, -volume = {124}, -year = {2002} -} - -@article{VanVelzen2013, -abstract = {Context. Many decades of observations of active galactic nuclei (AGN) and X-ray binaries have shown that relativistic jets are ubiquitous when compact objects accrete. One could therefore anticipate the launch of a jet after a star is disrupted and accreted by a massive black hole. This birth of a relativistic jet may have been observed recently in two stellar tidal disruption flares (TDFs), which were discovered in gamma-rays by Swift. Yet no transient radio emission has been detected from the tens of TDF candidates that were discovered at optical to soft X-ray frequencies. Because the sample that was followed-up at radio frequencies is small, the non-detections can be explained by Doppler boosting, which reduces the jet flux for off-axis observers. And since the existing follow-up observation are mostly within {\~{}}10 months of the discovery, the non-detections can also be due to a delay of the radio emission with respect to the time of disruption. Aims: We wish to test the conjecture that all TDFs launch jets. Methods: We present 5 GHz follow-up observations with the Jansky VLA of seven known TDFs, a significant increase of the number of radio observations of these events. To avoid missing delayed jet emission, our observations probe 1-8 years since the estimated time of disruption. Results: None of the sources are detected, with very deep upper limits at the 10 micro Jansky level. These observations rule out the hypothesis that these TDFs launched jets similar to radio-loud quasars. We also constrain the possibility that the flares hosted a jet identical to Sw 1644+57, the first and best-sampled relativistic TDF. Conclusions: We thus obtain evidence for a dichotomy in the stellar tidal disruption population, implying that the jet launching mechanism is sensitive to the parameters of the disruption.}, -author = {van Velzen, S. and Frail, D. A. and K{\"{o}}rding, E. and Falcke, H.}, -doi = {10.1051/0004-6361/201220426}, -issn = {0004-6361}, -journal = {Astronomy {\&} Astrophysics}, -keywords = {accretion,accretion disks,galaxies: jets,radiation mechanisms: non-thermal,radio continuum: general}, -month = {mar}, -pages = {A5}, -title = {{Constraints on off-axis jets from stellar tidal disruption flares}}, -url = {http://adsabs.harvard.edu/abs/2013A{\%}26A...552A...5V}, -volume = {552}, -year = {2013} -} - -@article{Cenko2012, -abstract = {We report the discovery by the Swift hard X-ray monitor of the transient source Swift J2058.4+0516 (Sw J2058+05). Our multi-wavelength follow-up campaign uncovered a long-lived (duration {\textgreater}{\~{}} months), luminous X-ray (L X, iso ≈ 3 × 1047 erg s-1) and radio ($\nu$L $\nu$, iso ≈ 1042 erg s-1) counterpart. The associated optical emission, however, from which we measure a redshift of 1.1853, is relatively faint, and this is not due to a large amount of dust extinction in the host galaxy. Based on numerous similarities with the recently discovered GRB 110328A/Swift J164449.3+573451 (Sw J1644+57), we suggest that Sw J2058+05 may be the second member of a new class of relativistic outbursts resulting from the tidal disruption of a star by a supermassive black hole. If so, the relative rarity of these sources (compared with the expected rate of tidal disruptions) implies that either these outflows are extremely narrowly collimated ($\theta$ {\textless} 1°) or only a small fraction of tidal disruptions generate relativistic ejecta. Analogous to the case of long-duration gamma-ray bursts and core-collapse supernovae, we speculate that rapid spin of the black hole may be a necessary condition to generate the relativistic component. Alternatively, if powered by gas accretion (i.e., an active galactic nucleus (AGN)), Sw J2058+05 would seem to represent a new mode of variability in these sources, as the observed properties appear largely inconsistent with known classes of AGNs capable of generating relativistic jets (blazars, narrow-line Seyfert 1 galaxies).}, -author = {{Bradley Cenko}, S. and Krimm, Hans A. and Horesh, Assaf and Rau, Arne and Frail, Dale A. and Kennea, Jamie A. and Levan, Andrew J. and Holland, Stephen T. and Butler, Nathaniel R. and Quimby, Robert M. and Bloom, Joshua S. and Filippenko, Alexei V. and Gal-Yam, Avishay and Greiner, Jochen and Kulkarni, S. R. and Ofek, Eran O. and {Olivares E.}, Felipe and Schady, Patricia and Silverman, Jeffrey M. and Tanvir, Nial R. and Xu, Dong}, -doi = {10.1088/0004-637X/753/1/77}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {X-rays: bursts,X-rays: individual: Sw J1644+57,accretion,accretion disks,black hole physics,galaxies: nuclei}, -month = {jul}, -number = {1}, -pages = {77}, -title = {{SWIFT J2058.4+0516: DISCOVERY OF A POSSIBLE SECOND RELATIVISTIC TIDAL DISRUPTION FLARE?}}, -url = {http://adsabs.harvard.edu/abs/2012ApJ...753...77C}, -volume = {753}, -year = {2012} -} - -@article{Svirski2015, -abstract = {Models for tidal disruption events (TDEs) in which a supermassive black hole disrupts a star commonly assume that the highly eccentric streams of bound stellar debris promptly form a circular accretion disk at the pericenter scale. However, the bolometric peak luminosity of most TDE candidates, {\$}\backslashsim10{\^{}}{\{}44{\}}\backslash,\backslashrm{\{}erg\backslash,s{\^{}}{\{}-1{\}}{\}}{\$}, implies that we observe only {\$}\backslashsim1\backslash{\%}{\$} of the energy expected from accretion. Moreover, recent numerical simulations (Shiokawa et al. 2015) have shown that dissipation via hydrodynamical shocks is insufficient to circularize debris orbits on the pericenter scale, and the debris flow retains its initial semi-major axis scale throughout the first {\$}\backslashsim10{\$} orbits of the event. Motivated by these numerical results, Piran et al. (2015) suggested that the observed optical TDE emission is powered by shocks at the apocenter between freshly infalling material and earlier-arriving matter. This model explains the small radiated energy, the low temperature, and the large radius implied by the observations as well as the {\$}t{\^{}}{\{}-5/3{\}}{\$} light curve. However the question of the system's low efficiency remains unanswered. We suggest that the high orbital energy and low angular momentum of the flow's highly eccentric orbits make it possible for magnetic stresses to reduce the matter's already small angular momentum to the point at which it can pass within the ISCO before these stresses remove enough energy to circularize the orbit. As a result, the typical efficiency is only {\$}\backslashsim3\backslash{\%}{\$} of a standard accretion disk's efficiency. Thus, the intrinsically high eccentricity of the tidal debris naturally explains why most TDE candidates are fainter than expected.}, -author = {Svirski, Gilad and Piran, Tsvi and Krolik, Julian}, -journal = {eprint arXiv:1508.02389}, -keywords = {Astrophysics - High Energy Astrophysical Phenomena}, -title = {{Inefficient highly eccentric accretion and the low luminosity of stellar tidal disruption events}}, -url = {http://adsabs.harvard.edu/abs/2015arXiv150802389S}, -year = {2015} -} - -@article{Lodato2009, -abstract = {In this paper, we revisit the arguments for the basis of the time evolution of the flares expected to arise when a star is disrupted by a supermassive black hole. We present a simple analytic model relating the light curve to the internal density structure of the star. We thus show that the standard light curve proportional to t-5/3 only holds at late times. Close to the peak luminosity the light curve is shallower, deviating more strongly from t-5/3 for more centrally concentrated (e.g. solar type) stars. We test our model numerically by simulating the tidal disruption of several stellar models, described by simple polytropic spheres with index $\gamma$. The simulations agree with the analytical model given two considerations. First, the stars are somewhat inflated on reaching pericentre because of the effective reduction of gravity in the tidal field of the black hole. This is well described by a homologous expansion by a factor which becomes smaller as the polytropic index becomes larger. Secondly, for large polytropic indices wings appear in the tails of the energy distribution, indicating that some material is pushed further away from parabolic orbits by shocks in the tidal tails. In all our simulations, the t-5/3 light curve is achieved only at late stages. In particular, we predict that for solar-type stars, this happens only after the luminosity has dropped by at least 2mag from the peak. We discuss our results in the light of recent observations of flares in otherwise quiescent galaxies and note the dependence of these results on further parameters, such as the star/hole mass ratio and the stellar orbit.}, -author = {Lodato, G. and King, A. R. and Pringle, J. E.}, -doi = {10.1111/j.1365-2966.2008.14049.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {black hole physics,galaxies: nuclei,hydrodynamics}, -month = {jan}, -number = {1}, -pages = {332--340}, -title = {{Stellar disruption by a supermassive black hole: is the light curve really proportional to t −5/3 ?}}, -url = {http://adsabs.harvard.edu/abs/2009MNRAS.392..332L}, -volume = {392}, -year = {2009} -} - -@article{Zauderer2011, -abstract = {Active galactic nuclei, which are powered by long-term accretion onto central supermassive black holes, produce relativistic jets with lifetimes of at least one million years, and the observation of the birth of such a jet is therefore unlikely. Transient accretion onto a supermassive black hole, for example through the tidal disruption of a stray star, thus offers a rare opportunity to study the birth of a relativistic jet. On 25 March 2011, an unusual transient source (Swift J164449.3+573451) was found, potentially representing such an accretion event. Here we report observations spanning centimetre to millimetre wavelengths and covering the first month of evolution of a luminous radio transient associated with Swift J164449.3+573451. The radio transient coincides with the nucleus of an inactive galaxy. We conclude that we are seeing a newly formed relativistic outflow, launched by transient accretion onto a million-solar-mass black hole. A relativistic outflow is not predicted in this situation, but we show that the tidal disruption of a star naturally explains the observed high-energy properties and radio luminosity and the inferred rate of such events. The weaker beaming in the radio-frequency spectrum relative to $\gamma$-rays or X-rays suggests that radio searches may uncover similar events out to redshifts of z ≈ 6.}, -author = {Zauderer, B A and Berger, E and Soderberg, A M and Loeb, A and Narayan, R and Frail, D A and Petitpas, G R and Brunthaler, A and Chornock, R and Carpenter, J M and Pooley, G G and Mooley, K and Kulkarni, S R and Margutti, R and Fox, D B and Nakar, E and Patel, N A and Volgenau, N H and Culverhouse, T L and Bietenholz, M F and Rupen, M P and Max-Moerbeck, W and Readhead, A C S and Richards, J and Shepherd, M and Storm, S and Hull, C L H}, -doi = {10.1038/nature10366}, -issn = {1476-4687}, -journal = {Nature}, -month = {aug}, -number = {7361}, -pages = {425--8}, -pmid = {21866155}, -title = {{Birth of a relativistic outflow in the unusual $\gamma$-ray transient Swift J164449.3+573451.}}, -url = {http://adsabs.harvard.edu/abs/2011Natur.476..425Z}, -volume = {476}, -year = {2011} -} - -@article{Gezari2006, -abstract = {A supermassive black hole in the nucleus of a galaxy will be revealed when a star passes close enough to be torn apart by tidal forces and a flare of radiation is emitted by the stream of stellar debris that plunges into the black hole. Since common active galactic nuclei have accreting black holes that can also produce flares, a convincing demonstration that a stellar tidal disruption has occurred generally begins with a ``normal'' galaxy that has no evidence of prior nuclear activity. Here we report a luminous UV flare from an elliptical galaxy at z=0.37 in the Groth field of the GALEX Deep Imaging Survey that has no evidence of a Seyfert nucleus from optical spectroscopy and X-ray imaging obtained during the flare. Multiwavelength data collected at the time of the event, and for 2 years following, allow us to constrain, for the first time, the spectral energy distribution of a candidate tidal disruption flare from optical through X-rays. The luminosity and temperature of the radiation and the decay curve of the flare are in excellent agreement with theoretical predictions for the tidal disruption of a star, and provide the strongest empirical evidence for a stellar disruption event to date.}, -author = {Gezari, S. and Martin, D. C. and Milliard, B. and Basa, S. and Halpern, J. P. and Forster, K. and Friedman, P. G. and Morrissey, P. and Neff, S. G. and Schiminovich, D. and Seibert, M. and Small, T. and Wyder, T. K.}, -doi = {10.1086/509918}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Nuclei,Ultraviolet: Galaxies}, -month = {dec}, -number = {1}, -pages = {L25--L28}, -title = {{Ultraviolet Detection of the Tidal Disruption of a Star by a Supermassive Black Hole}}, -url = {http://adsabs.harvard.edu/abs/2006ApJ...653L..25G}, -volume = {653}, -year = {2006} -} - -@article{VanVelzen2011, -abstract = {Using archival Sloan Digital Sky Survey (SDSS) multi-epoch imaging data (Stripe 82), we have searched for the tidal disruption of stars by supermassive black holes in non-active galaxies. Two candidate tidal disruption events (TDEs) are identified. The TDE flares have optical blackbody temperatures of 2 × 104 K and observed peak luminosities of Mg = -18.3 and -20.4 ($\nu$L $\nu$ = 5 × 1042, 4 × 1043 erg s-1, in the rest frame); their cooling rates are very low, qualitatively consistent with expectations for tidal disruption flares. The properties of the TDE candidates are examined using (1) SDSS imaging to compare them to other flares observed in the search, (2) UV emission measured by GALEX, and (3) spectra of the hosts and of one of the flares. Our pipeline excludes optically identifiable AGN hosts, and our variability monitoring over nine years provides strong evidence that these are not flares in hidden AGNs. The spectra and color evolution of the flares are unlike any SN observed to date, their strong late-time UV emission is particularly distinctive, and they are nuclear at high resolution arguing against these being first cases of a previously unobserved class of SNe or more extreme examples of known SN types. Taken together, the observed properties are difficult to reconcile with an SN or an AGN-flare explanation, although an entirely new process specific to the inner few hundred parsecs of non-active galaxies cannot be excluded. Based on our observed rate, we infer that hundreds or thousands of TDEs will be present in current and next-generation optical synoptic surveys. Using the approach outlined here, a TDE candidate sample with O(1) purity can be selected using geometric resolution and host and flare color alone, demonstrating that a campaign to create a large sample of TDEs, with immediate and detailed multi-wavelength follow-up, is feasible. A by-product of this work is quantification of the power spectrum of extreme flares in AGNs.}, -author = {van Velzen, Sjoert and Farrar, Glennys R. and Gezari, Suvi and Morrell, Nidia and Zaritsky, Dennis and {\"{O}}stman, Linda and Smith, Mathew and Gelfand, Joseph and Drake, Andrew J.}, -doi = {10.1088/0004-637X/741/2/73}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {black hole physics,galaxies: nuclei}, -month = {nov}, -number = {2}, -pages = {73}, -title = {{OPTICAL DISCOVERY OF PROBABLE STELLAR TIDAL DISRUPTION FLARES}}, -url = {http://adsabs.harvard.edu/abs/2011ApJ...741...73V}, -volume = {741}, -year = {2011} -} - -@article{Gezari2012, -abstract = {The flare of radiation from the tidal disruption and accretion of a star can be used as a marker for supermassive black holes that otherwise lie dormant and undetected in the centres of distant galaxies. Previous candidate flares have had declining light curves in good agreement with expectations, but with poor constraints on the time of disruption and the type of star disrupted, because the rising emission was not observed. Recently, two 'relativistic' candidate tidal disruption events were discovered, each of whose extreme X-ray luminosity and synchrotron radio emission were interpreted as the onset of emission from a relativistic jet. Here we report a luminous ultraviolet-optical flare from the nuclear region of an inactive galaxy at a redshift of 0.1696. The observed continuum is cooler than expected for a simple accreting debris disk, but the well-sampled rise and decay of the light curve follow the predicted mass accretion rate and can be modelled to determine the time of disruption to an accuracy of two days. The black hole has a mass of about two million solar masses, modulo a factor dependent on the mass and radius of the star disrupted. On the basis of the spectroscopic signature of ionized helium from the unbound debris, we determine that the disrupted star was a helium-rich stellar core.}, -author = {Gezari, S and Chornock, R and Rest, A and Huber, M E and Forster, K and Berger, E and Challis, P J and Neill, J D and Martin, D C and Heckman, T and Lawrence, A and Norman, C and Narayan, G and Foley, R J and Marion, G H and Scolnic, D and Chomiuk, L and Soderberg, A and Smith, K and Kirshner, R P and Riess, A G and Smartt, S J and Stubbs, C W and Tonry, J L and Wood-Vasey, W M and Burgett, W S and Chambers, K C and Grav, T and Heasley, J N and Kaiser, N and Kudritzki, R-P and Magnier, E A and Morgan, J S and Price, P A}, -doi = {10.1038/nature10990}, -issn = {1476-4687}, -journal = {Nature}, -month = {may}, -number = {7397}, -pages = {217--20}, -pmid = {22575962}, -title = {{An ultraviolet-optical flare from the tidal disruption of a helium-rich stellar core.}}, -url = {http://adsabs.harvard.edu/abs/2012Natur.485..217G}, -volume = {485}, -year = {2012} -} - -@article{Hills1975, -abstract = {The possible presence of massive black holes in the nuclei of galaxies has been suggested many times. In addition, there is considerable observational evidence for high stellar densities in these nuclei. I show that the tidal breakup of stars passing within the Roche limit of a black hole initiates a chain of events that may explain many of the observed principal characteristics of QSOs and the nuclei of Seyfert galaxies.}, -author = {Hills, J. G.}, -doi = {10.1038/254295a0}, -issn = {0028-0836}, -journal = {Nature}, -keywords = {Black Holes (Astronomy),Galactic Nuclei,Gas Flow,Mass Transfer,Quasars,Roche Limit,Seyfert Galaxies,Stellar Mass,Stellar Mass Ejection}, -month = {mar}, -number = {5498}, -pages = {295--298}, -title = {{Possible power source of Seyfert galaxies and QSOs}}, -url = {http://adsabs.harvard.edu/abs/1975Natur.254..295H}, -volume = {254}, -year = {1975} -} - -@article{Chornock2014, -abstract = {We present the Pan-STARRS1 discovery of the long-lived and blue transient PS1-11af, which was also detected by Galaxy Evolution Explorer with coordinated observations in the near-ultraviolet (NUV) band. PS1-11af is associated with the nucleus of an early type galaxy at redshift z = 0.4046 that exhibits no evidence for star formation or active galactic nucleus activity. Four epochs of spectroscopy reveal a pair of transient broad absorption features in the UV on otherwise featureless spectra. Despite the superficial similarity of these features to P-Cygni absorptions of supernovae (SNe), we conclude that PS1-11af is not consistent with the properties of known types of SNe. Blackbody fits to the spectral energy distribution are inconsistent with the cooling, expanding ejecta of a SN, and the velocities of the absorption features are too high to represent material in homologous expansion near a SN photosphere. However, the constant blue colors and slow evolution of the luminosity are similar to previous optically selected tidal disruption events (TDEs). The shape of the optical light curve is consistent with models for TDEs, but the minimum accreted mass necessary to power the observed luminosity is only {\~{}}0.002 M ⊙, which points to a partial disruption model. A full disruption model predicts higher bolometric luminosities, which would require most of the radiation to be emitted in a separate component at high energies where we lack observations. In addition, the observed temperature is lower than that predicted by pure accretion disk models for TDEs and requires reprocessing to a constant, lower temperature. Three deep non-detections in the radio with the Very Large Array over the first two years after the event set strict limits on the production of any relativistic outflow comparable to Swift J1644+57, even if off-axis.}, -author = {Chornock, R. and Berger, E. and Gezari, S. and Zauderer, B. A. and Rest, A. and Chomiuk, L. and Kamble, A. and Soderberg, A. M. and Czekala, I. and Dittmann, J. and Drout, M. and Foley, R. J. and Fong, W. and Huber, M. E. and Kirshner, R. P. and Lawrence, A. and Lunnan, R. and Marion, G. H. and Narayan, G. and Riess, A. G. and Roth, K. C. and Sanders, N. E. and Scolnic, D. and Smartt, S. J. and Smith, K. and Stubbs, C. W. and Tonry, J. L. and Burgett, W. S. and Chambers, K. C. and Flewelling, H. and Hodapp, K. W. and Kaiser, N. and Magnier, E. A. and Martin, D. C. and Neill, J. D. and Price, P. A. and Wainscoat, R.}, -doi = {10.1088/0004-637X/780/1/44}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {accretion,accretion disks,black hole physics,galaxies: nuclei}, -month = {jan}, -number = {1}, -pages = {44}, -title = {{THE ULTRAVIOLET-BRIGHT, SLOWLY DECLINING TRANSIENT PS1-11af AS A PARTIAL TIDAL DISRUPTION EVENT}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...780...44C}, -volume = {780}, -year = {2014} -} - -@article{Piran2015, -abstract = {A tidal disruption event (TDE) takes place when a star passes near enough to a massive black hole to be disrupted. About half the star's matter is given elliptical trajectories with large apocenter distances, and the other half is unbound. To form an accretion flow, the bound matter must lose a significant amount of energy, with the actual amount depending on the characteristic scale of the flow measured in units of the black hole's gravitational radius (˜ {\{}{\{}10{\}}51{\}}{\{}{\{}(R/1000{\{}{\{}R{\}}g{\}}){\}}-1{\}} erg). Recent numerical simulations have revealed that the accretion flow scale is close to the scale of the most bound initial orbits, ˜ {\{}{\{}10{\}}3{\}}MBH,6.5-2/3{\{}{\{}R{\}}g{\}}˜ {\{}{\{}10{\}}15{\}}MBH,6.51/3 cm from the black hole, and the corresponding energy dissipation rate is ˜ {\{}{\{}10{\}}44{\}}MBH,6.5-1/6 erg s-1. We suggest that the energy liberated during the formation of the accretion disk, rather than the energy liberated by subsequent accretion onto the black hole, powers the observed optical TDE candidates. The observed rise times, luminosities, temperatures, emission radii, and line widths seen in these TDEs are all more readily explained in terms of heating associated with disk formation rather than in terms of accretion.}, -author = {Piran, Tsvi and Svirski, Gilad and Krolik, Julian and Cheng, Roseanne M. and Shiokawa, Hotaka}, -doi = {10.1088/0004-637X/806/2/164}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {accretion,accretion disks,black hole physics,galaxies: nuclei,stars: black holes}, -month = {jun}, -number = {2}, -pages = {164}, -title = {{DISK FORMATION VERSUS DISK ACCRETION—WHAT POWERS TIDAL DISRUPTION EVENTS?}}, -url = {http://adsabs.harvard.edu/abs/2015ApJ...806..164P}, -volume = {806}, -year = {2015} -} - -@article{Strubbe2015, -abstract = {Was PS1-10jh, an optical/ultraviolet transient discovered by the Pan-STARRS Medium Deep Survey, the tidal disruption of a star by a massive black hole (BH)? We address two aspects of the problem: the composition of the putative disrupted object (using the spectroscopic data), and the energetics of the observed gas and radiation (using the photometric data). We perform photoionization calculations and compare with the observed lower limit of the line ratio L{\_}{\{}He II 4686{\}}/L{\_}{\{}H$\alpha$ {\}}{\textgreater}5 to argue that this event was not the disruption of a solar-type star, and instead was likely the disruption of a helium core (as first proposed by Gezari et al.). Disruption of such a dense object requires a relatively small central BH, MBH ≲ 2 × 105 M⊙. We use the photometric data to infer that PS1-10jh comprised an outflow of ˜0.01 M⊙ of gas, escaping from the BH at ˜1000 km s-1, and we propose that this outflow was driven primarily by radiation pressure trapped by Thomson and resonance line scattering. The large ratio of radiated energy to kinetic energy, Erad/EK ˜ 104, together with the large value of Erad ˜ 2 × 1051 erg, suggests that the outflow was shocked at large radius (perhaps similar to superluminous supernovae or the internal shock model for gamma-ray bursts). We describe puzzles in the physics of PS1-10jh, and discuss how this event may help us understand future tidal disruptions and super-Eddington accretion events as well.}, -author = {Strubbe, Linda E. and Murray, Norman}, -doi = {10.1093/mnras/stv2081}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {black hole physics,galaxies: nuclei}, -month = {oct}, -number = {3}, -pages = {2321--2343}, -title = {{Insights into tidal disruption of stars from PS1-10jh}}, -url = {http://adsabs.harvard.edu/abs/2015MNRAS.454.2321S}, -volume = {454}, -year = {2015} -} - -@article{Stone2015, -abstract = {Rates of stellar tidal disruption events (TDEs) by supermassive black holes (SMBHs) due to two-body relaxation are calculated using a large galaxy sample (N ≈ 200) in order to explore the sensitivity of the TDE rates to observational uncertainties, such as the parametrization of galaxy light profiles and the stellar mass function. The largest uncertainty arises due to the poorly constrained occupation fraction of SMBHs in low-mass galaxies, which otherwise dominate the total TDE rate. The detection rate of TDE flares by optical surveys is calculated as a function of SMBH mass and other observables for several physically motivated models of TDE emission. We also quantify the fraction of galaxies that produce deeply penetrating disruption events. If the majority of the detected events are characterized by super-Eddington luminosities (such as disc winds, or synchrotron radiation from an off-axis relativistic jet), then the measured SMBH mass distribution will tightly constrain the low-end SMBH occupation fraction. If Eddington-limited emission channels dominate, however, then the occupation fraction sensitivity is much less pronounced in a flux-limited survey (although still present in a volume-complete event sample). The SMBH mass distribution of the current sample of TDEs, though highly inhomogeneous and encumbered by selection effects, already suggests that Eddington-limited emission channels dominate. Even our most conservative rate estimates appear to be in tension with much lower observationally inferred TDE rates, and we discuss several possible resolutions to this discrepancy.}, -author = {Stone, N. C. and Metzger, B. D.}, -doi = {10.1093/mnras/stv2281}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {X-rays: bursts,accretion,accretion discs,black hole physics,galaxies: nuclei}, -month = {nov}, -number = {1}, -pages = {859--883}, -title = {{Rates of stellar tidal disruption as probes of the supermassive black hole mass function}}, -url = {http://adsabs.harvard.edu/abs/2016MNRAS.455..859S}, -volume = {455}, -year = {2015} -} - -@article{Holoien2015, -abstract = {We present ground-based and Swift photometric and spectroscopic observations of the candidate tidal disruption event (TDE) ASASSN-14li, found at the centre of PGC 043234 (d ≃ 90 Mpc) by the All-Sky Automated Survey for SuperNovae (ASAS-SN). The source had a peak bolometric luminosity of L ≃ 1044 erg s-1 and a total integrated energy of E ≃ 7 × 1050 erg radiated over the ˜6 months of observations presented. The UV/optical emission of the source is well fitted by a blackbody with roughly constant temperature of T ˜ 35 000 K, while the luminosity declines by roughly a factor of 16 over this time. The optical/UV luminosity decline is broadly consistent with an exponential decline, L∝ e{\^{}}{\{}-t/t{\_}0{\}}, with t0 ≃ 60 d. ASASSN-14li also exhibits soft X-ray emission comparable in luminosity to the optical and UV emission but declining at a slower rate, and the X-ray emission now dominates. Spectra of the source show broad Balmer and helium lines in emission as well as strong blue continuum emission at all epochs. We use the discoveries of ASASSN-14li and ASASSN-14ae to estimate the TDE rate implied by ASAS-SN, finding an average rate of r ≃ 4.1 × 10-5 yr-1 per galaxy with a 90 per cent confidence interval of (2.2-17.0) × 10-5 yr-1 per galaxy. ASAS-SN found roughly 1 TDE for every 70 Type Ia supernovae in 2014, a rate that is much higher than that of other surveys.}, -author = {Holoien, T. W.-S. and Kochanek, C. S. and Prieto, J. L. and Stanek, K. Z. and Dong, Subo and Shappee, B. J. and Grupe, D. and Brown, J. S. and Basu, U. and Beacom, J. F. and Bersier, D. and Brimacombe, J. and Danilet, A. B. and Falco, E. and Guo, Z. and Jose, J. and Herczeg, G. J. and Long, F. and Pojmanski, G. and Simonian, G. V. and Szczygie{\l}, D. M. and Thompson, T. A. and Thorstensen, J. R. and Wagner, R. M. and Wo{\'{z}}niak, P. R.}, -doi = {10.1093/mnras/stv2486}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {accretion,accretion discs,black hole physics,galaxies: nuclei}, -month = {nov}, -number = {3}, -pages = {2918--2935}, -title = {{Six months of multiwavelength follow-up of the tidal disruption candidate ASASSN-14li and implied TDE rates from ASAS-SN}}, -url = {http://adsabs.harvard.edu/abs/2016MNRAS.455.2918H}, -volume = {455}, -year = {2015} -} - -@article{Wang2004, -abstract = {We compute rates of tidal disruption of stars by supermassive black holes in galactic nuclei, using downwardly revised black hole masses from the MBH-$\sigma$ relation. In galaxies with steep nuclear density profiles, which dominate the overall event rate, the disruption frequency varies inversely with assumed black hole mass. We compute a total rate for nondwarf galaxies of {\~{}}10-5 yr-1 Mpc-3, about a factor of 10 higher than in earlier studies. Disruption rates are predicted to be highest in nucleated dwarf galaxies, assuming that such galaxies contain black holes. Monitoring of a rich galaxy cluster for a few years could rule out the existence of intermediate-mass black holes in dwarf galaxies.}, -author = {Wang, Jianxiang and Merritt, David}, -doi = {10.1086/379767}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Dwarf,Galaxies: Kinematics and Dynamics,Galaxies: Nuclei,Stellar Dynamics}, -month = {jan}, -number = {1}, -pages = {149--161}, -title = {{Revised Rates of Stellar Disruption in Galactic Nuclei}}, -url = {http://adsabs.harvard.edu/abs/2004ApJ...600..149W}, -volume = {600}, -year = {2004} -} - -@article{Roth2015, -abstract = {Observations of luminous flares resulting from the possible tidal disruption of stars by supermassive black holes have raised a number of puzzles. Outstanding questions include the origin of the optical and ultraviolet (UV) flux, the weakness of hydrogen lines in the spectrum, and the occasional simultaneous observation of x-rays. Here we study the emission from tidal disruption events (TDEs) produced as radiation from black hole accretion propagates through an extended, optically thick envelope formed from stellar debris. We analytically describe key physics controlling spectrum formation, and present detailed radiative transfer calculations that model the spectral energy distribution (SED) and optical line strengths of TDEs near peak brightness. The steady-state transfer is coupled to a non local thermodynamic equilibrium treatment of the excitation and ionization states of hydrogen, helium and oxygen (as a representative metal). Our calculations show how an extended envelope can reprocess a fraction of soft x-rays and produce the observed optical fluxes of order 10{\^{}}43 ergs per second. Variations in the mass or size of the envelope may help explain how the optical flux changes over time with roughly constant color. For high enough accretion luminosities, x-rays can highly ionize the reprocessing region and escape to be observed simultaneously with the optical flux, producing an SED not described by a single blackbody. Due to optical depth effects, hydrogen Balmer line emission is often strongly suppressed relative to helium line emission (with HeII-to-H line ratios of at least 5:1 in some cases) even in the disruption of a solar-composition star. We discuss the implications of our results to understanding the type of stars destroyed in TDEs and the physical processes responsible for producing the observed flares.}, -author = {Roth, Nathaniel and Kasen, Daniel and Guillochon, James and Ramirez-Ruiz, Enrico}, -journal = {eprint arXiv:1510.08454}, -keywords = {Astrophysics - High Energy Astrophysical Phenomena}, -title = {{The X-ray through Optical Fluxes and Line Strengths of Tidal Disruption Events}}, -url = {http://adsabs.harvard.edu/abs/2015arXiv151008454R}, -year = {2015} -} - -@article{Holoien2014, -abstract = {ASASSN-14ae is a candidate tidal disruption event (TDE) found at the centre of SDSS J110840.11+340552.2 (d ≃ 200 Mpc) by the All-Sky Automated Survey for Supernovae (ASAS-SN). We present ground-based and Swift follow-up photometric and spectroscopic observations of the source, finding that the transient had a peak luminosity of L ≃ 8 × 1043 erg s-1 and a total integrated energy of E ≃ 1.7 × 1050 erg radiated over the ˜5 months of observations presented. The blackbody temperature of the transient remains roughly constant at T ˜ 20 000 K while the luminosity declines by nearly 1.5 orders of magnitude during this time, a drop that is most consistent with an exponential, L ∝ e-t/t 0 with t0 ≃ 39 d. The source has broad Balmer lines in emission at all epochs as well as a broad He II feature emerging in later epochs. We compare the colour and spectral evolution to both supernovae and normal AGN to show that ASASSN-14ae does not resemble either type of object and conclude that a TDE is the most likely explanation for our observations. At z = 0.0436, ASASSN-14ae is the lowest-redshift TDE candidate discovered at optical/UV wavelengths to date, and we estimate that ASAS-SN may discover 0.1-3 of these events every year in the future.}, -author = {Holoien, T. W.- S. and Prieto, J. L. and Bersier, D. and Kochanek, C. S. and Stanek, K. Z. and Shappee, B. J. and Grupe, D. and Basu, U. and Beacom, J. F. and Brimacombe, J. and Brown, J. S. and Davis, A. B. and Jencson, J. and Pojmanski, G. and Szczygie , D. M.}, -doi = {10.1093/mnras/stu1922}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {accretion,accretion discs,black hole physics,galaxies: nuclei}, -month = {oct}, -number = {3}, -pages = {3263--3277}, -title = {{ASASSN-14ae: a tidal disruption event at 200 Mpc}}, -url = {http://adsabs.harvard.edu/abs/2014MNRAS.445.3263H}, -volume = {445}, -year = {2014} -} - -@article{Brown2015, -abstract = {We present observations of Swift J1112.2-8238, and identify it as a candidate relativistic tidal disruption flare. The outburst was first detected by Swift/Burst Alert Telescope (BAT) in 2011 June as an unknown, long-lived (order of days) gamma-ray transient source. We show that its position is consistent with the nucleus of a faint galaxy for which we establish a likely redshift of z = 0.89 based on a single emission line that we interpret as the blended [O II] $\lambda$3727 doublet. At this redshift, the peak X-ray/gamma-ray luminosity exceeded 1047 erg s-1, while a spatially coincident optical transient source had i' ˜ 22 (Mg ˜ -21.4 at z = 0.89) during early observations, ˜20 d after the Swift trigger. These properties place Swift J1112.2-8238 in a very similar region of parameter space to the two previously identified members of this class, Swift J1644+57 and Swift J2058+0516. As with those events the high-energy emission shows evidence for variability over the first few days, while late-time observations, almost 3 yr post-outburst, demonstrate that it has now switched off. Swift J1112.2-8238 brings the total number of such events observed by Swift to three, interestingly all detected by Swift over a ˜3 month period ({\textless}3 per cent of its total lifetime as of 2015 March). While this suggests the possibility that further examples may be uncovered by detailed searches of the BAT archives, the lack of any prime candidates in the years since 2011 means these events are undoubtedly rare.}, -author = {Brown, G. C. and Levan, A. J. and Stanway, E. R. and Tanvir, N. R. and Cenko, S. B. and Berger, E. and Chornock, R. and Cucchiaria, A.}, -doi = {10.1093/mnras/stv1520}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {galaxies: nuclei,gamma-rays: galaxies}, -month = {aug}, -number = {4}, -pages = {4297--4306}, -title = {{Swift J1112.2−8238: a candidate relativistic tidal disruption flare}}, -url = {http://adsabs.harvard.edu/abs/2015MNRAS.452.4297B}, -volume = {452}, -year = {2015} -} - -@article{Bloom2011, -abstract = {Gas accretion onto some massive black holes (MBHs) at the centers of galaxies actively powers luminous emission, but most MBHs are considered dormant. Occasionally, a star passing too near an MBH is torn apart by gravitational forces, leading to a bright tidal disruption flare (TDF). Although the high-energy transient Sw 1644+57 initially displayed none of the theoretically anticipated (nor previously observed) TDF characteristics, we show that observations suggest a sudden accretion event onto a central MBH of mass about 10(6) to 10(7) solar masses. There is evidence for a mildly relativistic outflow, jet collimation, and a spectrum characterized by synchrotron and inverse Compton processes; this leads to a natural analogy of Sw 1644+57 to a temporary smaller-scale blazar.}, -author = {Bloom, Joshua S and Giannios, Dimitrios and Metzger, Brian D and Cenko, S Bradley and Perley, Daniel A and Butler, Nathaniel R and Tanvir, Nial R and Levan, Andrew J and O'Brien, Paul T and Strubbe, Linda E and {De Colle}, Fabio and Ramirez-Ruiz, Enrico and Lee, William H and Nayakshin, Sergei and Quataert, Eliot and King, Andrew R and Cucchiara, Antonino and Guillochon, James and Bower, Geoffrey C and Fruchter, Andrew S and Morgan, Adam N and van der Horst, Alexander J}, -doi = {10.1126/science.1207150}, -issn = {1095-9203}, -journal = {Science (New York, N.Y.)}, -month = {jul}, -number = {6039}, -pages = {203--6}, -pmid = {21680812}, -title = {{A possible relativistic jetted outburst from a massive black hole fed by a tidally disrupted star.}}, -url = {http://adsabs.harvard.edu/abs/2011Sci...333..203B}, -volume = {333}, -year = {2011} -} - -@article{Levan2011, -abstract = {Variable x-ray and $\gamma$-ray emission is characteristic of the most extreme physical processes in the universe. We present multiwavelength observations of a unique $\gamma$-ray-selected transient detected by the Swift satellite, accompanied by bright emission across the electromagnetic spectrum, and whose properties are unlike any previously observed source. We pinpoint the event to the center of a small, star-forming galaxy at redshift z = 0.3534. Its high-energy emission has lasted much longer than any $\gamma$-ray burst, whereas its peak luminosity was ∼100 times higher than bright active galactic nuclei. The association of the outburst with the center of its host galaxy suggests that this phenomenon has its origin in a rare mechanism involving the massive black hole in the nucleus of that galaxy.}, -author = {Levan, A J and Tanvir, N R and Cenko, S B and Perley, D A and Wiersema, K and Bloom, J S and Fruchter, A S and Postigo, A de Ugarte and O'Brien, P T and Butler, N and van der Horst, A J and Leloudas, G and Morgan, A N and Misra, K and Bower, G C and Farihi, J and Tunnicliffe, R L and Modjaz, M and Silverman, J M and Hjorth, J and Th{\"{o}}ne, C and Cucchiara, A and Cer{\'{o}}n, J M Castro and Castro-Tirado, A J and Arnold, J A and Bremer, M and Brodie, J P and Carroll, T and Cooper, M C and Curran, P A and Cutri, R M and Ehle, J and Forbes, D and Fynbo, J and Gorosabel, J and Graham, J and Hoffman, D I and Guziy, S and Jakobsson, P and Kamble, A and Kerr, T and Kasliwal, M M and Kouveliotou, C and Kocevski, D and Law, N M and Nugent, P E and Ofek, E O and Poznanski, D and Quimby, R M and Rol, E and Romanowsky, A J and S{\'{a}}nchez-Ram{\'{i}}rez, R and Schulze, S and Singh, N and van Spaandonk, L and Starling, R L C and Strom, R G and Tello, J C and Vaduvescu, O and Wheatley, P J and Wijers, R A M J and Winters, J M and Xu, D}, -doi = {10.1126/science.1207143}, -issn = {1095-9203}, -journal = {Science (New York, N.Y.)}, -month = {jul}, -number = {6039}, -pages = {199--202}, -pmid = {21680811}, -title = {{An extremely luminous panchromatic outburst from the nucleus of a distant galaxy.}}, -url = {http://adsabs.harvard.edu/abs/2011Sci...333..199L}, -volume = {333}, -year = {2011} -} - -@article{Rees1988, -abstract = {Stars in galactic nuclei can be captured or tidally disrupted by a central black hole. Some debris would be ejected at high speed; the remainder would be swallowed by the hole, causing a bright flare lasting at most a few years. Such phenomena are compatible with the presence of 10 to the 6th-10 to the 8th solar mass holes in the nuclei of many nearby galaxies. Stellar disruption may have interesting consequences in our own Galactic Center if an approximately 10 to the 6th solar mass hole lurks there.}, -author = {Rees, Martin J.}, -doi = {10.1038/333523a0}, -issn = {0028-0836}, -journal = {Nature}, -keywords = {Active Galactic Nuclei,Black Holes (Astronomy),Quasars,Red Shift,Star Distribution,Stellar Flares,Stellar Mass,Tides}, -month = {jun}, -number = {6173}, -pages = {523--528}, -title = {{Tidal disruption of stars by black holes of 106–108 solar masses in nearby galaxies}}, -url = {http://adsabs.harvard.edu/abs/1988Natur.333..523R}, -volume = {333}, -year = {1988} -} - -@article{Guillochon2014, -abstract = {When a star comes within a critical distance to a supermassive black hole (SMBH), immense tidal forces disrupt the star, resulting in a stream of debris that falls back onto the SMBH and powers a luminous flare. In this paper, we perform hydrodynamical simulations of the disruption of a main-sequence star by an SMBH to characterize the evolution of the debris stream after a tidal disruption. We demonstrate that this debris stream is confined by self-gravity in the two directions perpendicular to the original direction of the star's travel and as a consequence has a negligible surface area and makes almost no contribution to either the continuum or line emission. We therefore propose that any observed emission lines are not the result of photoionization in this unbound debris, but are produced in the region above and below the forming elliptical accretion disk, analogous to the broad-line region (BLR) in steadily accreting active galactic nuclei. As each line within a BLR is observationally linked to a particular location in the accretion disk, we suggest that the absence of a line indicates that the accretion disk does not yet extend to the distance required to produce that line. This model can be used to understand the spectral properties of the tidal disruption event PS1-10jh, for which He II lines are observed, but the Balmer series and He I are not. Using a maximum likelihood analysis, we show that the disruption of a main-sequence star of near-solar composition can reproduce this event.}, -author = {Guillochon, James and Manukian, Haik and Ramirez-Ruiz, Enrico}, -doi = {10.1088/0004-637X/783/1/23}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {accretion,accretion disks,black hole physics,galaxies: active,gravitational lensing: weak,hydrodynamics,methods: numerical}, -month = {mar}, -number = {1}, -pages = {23}, -title = {{PS1-10jh: THE DISRUPTION OF A MAIN-SEQUENCE STAR OF NEAR-SOLAR COMPOSITION}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...783...23G}, -volume = {783}, -year = {2014} -} - -@article{Hayasaki2015, -abstract = {We study the circularization of tidally disrupted stars on bound orbits around spinning supermassive black holes by performing three-dimensional smoothed particle hydrodynamic simulations with Post-Newtonian corrections. Our simulations reveal that debris circularization depends sensitively on the efficiency of radiative cooling. There are two stages in debris circularization if radiative cooling is inefficient: first, the stellar debris streams self-intersect due to relativistic apsidal precession; shocks at the intersection points thermalize orbital energy and the debris forms a geometrically thick, ring-like structure around the black hole. The ring rapidly spreads via viscous diffusion, leading to the formation of a geometrically thick accretion disk. In contrast, if radiative cooling is efficient, the stellar debris circularizes due to self-intersection shocks and forms a geometrically thin ring-like structure. In this case, the dissipated energy can be emitted during debris circularization as a precursor to the subsequent tidal disruption flare. The possible radiated energy is up to {\~{}}2*10{\^{}}{\{}52{\}} erg for a 1 Msun star orbiting a 10{\^{}}6 Msun black hole. We also find that a retrograde (prograde) black hole spin causes the shock-induced circularization timescale to be shorter (longer) than that of a non-spinning black hole in both cooling cases. The circularization timescale is remarkably long in the radiatively efficient cooling case, and is also sensitive to black hole spin. Specifically, Lense-Thirring torques cause dynamically important nodal precession, which significantly delays debris circularization. On the other hand, nodal precession is too slow to produce observable signatures in the radiatively inefficient case. We also discuss the relationship between our simulations and the parabolic TDEs that are characteristic of most stellar tidal disruptions.}, -author = {Hayasaki, Kimitake and Stone, Nicholas C. and Loeb, Abraham}, -journal = {eprint arXiv:1501.05207}, -keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - High Energy Astrophysical Phenomena}, -title = {{Circularization of Tidally Disrupted Stars around Spinning Supermassive Black Holes}}, -url = {http://adsabs.harvard.edu/abs/2015arXiv150105207H}, -year = {2015} -} - -@article{Esquej2007, -abstract = {Context: In recent years, giant amplitude X-ray flares have been observed from a handful of non-active galaxies. The most plausible scenario of these unusual phenomena is tidal disruption of a star by a quiescent supermassive black hole at the centre of the galaxy. Aims: Only a small number of these type of events have been observed and confirmed to date. The discovery of more cases would allow a number of fundamental conclusions to be drawn about properties such as the frequency of tidal disruption events, the distribution of quiescent black hole masses and their influence in the context of galaxy/AGN formation and evolution among others. Methods: Comparing the XMM-Newton Slew Survey Source Catalogue with the ROSAT PSPC All-Sky Survey five galaxies have been detected a factor of up to 88 brighter in XMM-Newton with respect to ROSAT PSPC upper limits and presenting a soft X-ray colour. X-ray luminosities of these sources derived from slew observations have been found in the range 1041{\{}-{\}}1044 erg s-1, fully consistent with the tidal disruption model. This model predicts that during the peak of the outburst, flares reach X-ray luminosities up to 1045 erg s-1, which is close to the Eddington luminosity of the black hole, and afterwards a decay of the flux on a time scale of months to years is expected. Multi-wavelength follow-up observations have been performed on these highly variable objects in order to disentangle their nature and to investigate their dynamical evolution. Results: Here we present sources coming from the XMM-Newton Slew Survey that could fit in the paradigm of tidal disruption events. X-ray and optical observations revealed that two of these objects are in full agreement with that scenario and three other sources that, showing signs of optical activity, need further investigation within the transient galactic nuclei phenomena.}, -author = {Esquej, P. and Saxton, R. D. and Freyberg, M. J. and Read, A. M. and Altieri, B. and Sanchez-Portal, M. and Hasinger, G.}, -doi = {10.1051/0004-6361:20066072}, -issn = {0004-6361}, -journal = {Astronomy and Astrophysics}, -keywords = {X-rays: general,galaxies: general,surveys}, -month = {feb}, -number = {3}, -pages = {L49--L52}, -title = {{Candidate tidal disruption events from the XMM-Newton slew survey}}, -url = {http://adsabs.harvard.edu/abs/2007A{\%}26A...462L..49E}, -volume = {462}, -year = {2007} -} - -@ARTICLE{2014Natur.509..471G, - author = {{Gal-Yam}, A. and {Arcavi}, I. and {Ofek}, E.~O. and {Ben-Ami}, S. and - {Cenko}, S.~B. and {Kasliwal}, M.~M. and {Cao}, Y. and {Yaron}, O. and - {Tal}, D. and {Silverman}, J.~M. and {Horesh}, A. and {De Cia}, A. and - {Taddia}, F. and {Sollerman}, J. and {Perley}, D. and {Vreeswijk}, P.~M. and - {Kulkarni}, S.~R. and {Nugent}, P.~E. and {Filippenko}, A.~V. and - {Wheeler}, J.~C.}, - title = "{A Wolf-Rayet-like progenitor of SN 2013cu from spectral observations of a stellar wind}", - journal = {\nat}, -archivePrefix = "arXiv", - 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Predicting Stellar Angular Diameters}", - journal = {\aj}, -archivePrefix = "arXiv", - eprint = {1311.4901}, - primaryClass = "astro-ph.SR", - keywords = {Hertzsprung-Russell and C-M diagrams, planetary systems, stars: early-type, stars: fundamental parameters, stars: general, stars: late-type}, - year = 2014, - month = mar, - volume = 147, - eid = {47}, - pages = {47}, - doi = {10.1088/0004-6256/147/3/47}, - adsurl = {http://adsabs.harvard.edu/abs/2014AJ....147...47B}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - -@INPROCEEDINGS{2013AAS...22124710S, - author = {{Shemmer}, O. and {Anderson}, S.~F. and {Ballantyne}, D.~R. and - {Barth}, A.~J. and {Brandt}, W.~N. and {Brunner}, R.~J. and - {Chartas}, G. and {Coppi}, P.~S. and {de Vries}, W.~H. and {Eracleous}, M. and - {Fan}, X. and {Gibson}, R. and {Gray}, A.~G. and {Green}, R.~F. and - {Kimball}, A.~E. and {Lacy}, M. and {Lira}, P. and {Madejski}, G.~M. and - {Newman}, J. and {Richards}, G.~T. and {Schneider}, D.~P. and - {Seth}, A. and {Smith}, H.~A. and {Strauss}, M.~A. and {Treister}, E. and - {Trouille}, L. and {Urry}, C.~M. and {Vanden Berk}, D.}, - title = "{AGN Science with the LSST}", -booktitle = {American Astronomical Society Meeting Abstracts \#221}, - year = 2013, - series = {American Astronomical Society Meeting Abstracts}, - volume = 221, - month = jan, - eid = {247.10}, - pages = {247.10}, - adsurl = {http://adsabs.harvard.edu/abs/2013AAS...22124710S}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} From 5f4573c77a797a91629dfe5b9c1aaa6b506467b6 Mon Sep 17 00:00:00 2001 From: Phil Marshall Date: Sun, 16 Sep 2018 19:18:22 -0400 Subject: [PATCH 2/6] Update to Sept 2018 --- whitepaper/preface.tex | 16 ++++++++-------- 1 file changed, 8 insertions(+), 8 deletions(-) diff --git a/whitepaper/preface.tex b/whitepaper/preface.tex index 57e8cd4..a7c1c9d 100644 --- a/whitepaper/preface.tex +++ b/whitepaper/preface.tex @@ -32,24 +32,24 @@ \chapter*{Preface} cases, and so enable good decisions to be made when the telescope schedule is eventually set up. -\noindent This white paper is a compendium of ideas and results +\noindent This community observing strategy evaluation paper (COSEP) is a compendium of ideas and results generated by the community, assembled so that everyone can follow along with the analysis. It is a living document, whose purpose is to bind together the group of people who are thinking about the LSST observing strategy problem, and facilitate their collective discussion and understanding of that problem (a process we might think of as ``cadence diplomacy''). Its audience is the LSST science community, and most notable its Science -Advisory Committee and Project Scientist who together will in the end decide what the LSST observing strategy will be. This white paper is {\it +Advisory Committee (SAC) and Project Scientist who together will in the end decide what the initial LSST observing strategy will be. This paper is {\it the} vehicle for the community to communicate to the LSST Project, while -the baseline observing strategy continues to be improved. +the baseline observing strategy continues to be improved. In June 2018 the LSST Project issued a call for white papers on LSST cadence optimization, that will lead to a number of new science-motivated observing strategy designs for the SAC to review, and recommend to the Project for simulation during 2019. Evaluation of those simulations in 2020 will inform the SAC's Survey Strategy Committee as it makes its recommendation for the initial LSST survey strategy in early 2021. -\noindent The white paper's modular design allows pieces of it to be +\noindent The COSEP's modular design allows pieces of it to be split off and published in a series of snapshot journal papers, as the -various metric analyses reach maturity. The white paper itself will be +various metric analyses reach maturity. The COSEP itself will be continuously published on \href{https://github.com/LSSTScienceCollaborations/ObservingStrategy}{\GitHub} and advertized periodically on \href{http://arxiv.org}{astro-ph}. This -white paper is large, but we hope that its hyperlinked structure helps +paper is large, but we hope that its hyperlinked structure helps our community quickly find the science cases that they are most interested in, starting from the \hyperref[toc]{table of contents}. @@ -59,7 +59,7 @@ \chapter*{Preface} \vspace{2\baselineskip} -{\raggedleft \credit{drphilmarshall}, \credit{ivezic} and \credit{bethwillman} \\ - \medskip \hspace{0.8\linewidth} \it August 12, 2017.} +{\raggedleft \credit{drphilmarshall}, \credit{ivezic} and \credit{rhiannonlynne} \\ + \medskip \hspace{0.8\linewidth} \it September 16, 2018.} \clearpage From 608a8585107b565826eccb2ede740193a55b9730 Mon Sep 17 00:00:00 2001 From: Phil Marshall Date: Sun, 16 Sep 2018 19:23:39 -0400 Subject: [PATCH 3/6] Small advance while we get set up for v2 --- whitepaper/Makefile | 2 +- 1 file changed, 1 insertion(+), 1 deletion(-) diff --git a/whitepaper/Makefile b/whitepaper/Makefile index 2588e83..81f1ae5 100644 --- a/whitepaper/Makefile +++ b/whitepaper/Makefile @@ -23,7 +23,7 @@ LSST_Observing_Strategy_White_Paper.pdf: version LSST_Observing_Strategy_White_P pdflatex LSST_Observing_Strategy_White_Paper.tex version: - tcsh gen_version.csh --version 1.0 + tcsh gen_version.csh --version 1.1 run: $(ARG)_standalone.tex LSST_Observing_Strategy_White_Paper.sty $(BIBFILES) $(TEXFILES) pdflatex $(ARG)_standalone.tex From ccd981e16fc9dac72902404015d9fa7f91c731a9 Mon Sep 17 00:00:00 2001 From: Phil Marshall Date: Mon, 17 Sep 2018 00:40:59 -0400 Subject: [PATCH 4/6] Possible structure for capturing the 2018 white paper content --- .../LSST_Observing_Strategy_White_Paper.tex | 55 +++++++++++-------- 1 file changed, 32 insertions(+), 23 deletions(-) diff --git a/whitepaper/LSST_Observing_Strategy_White_Paper.tex b/whitepaper/LSST_Observing_Strategy_White_Paper.tex index ec9eb9c..e4c328c 100644 --- a/whitepaper/LSST_Observing_Strategy_White_Paper.tex +++ b/whitepaper/LSST_Observing_Strategy_White_Paper.tex @@ -65,51 +65,60 @@ % -------------------------------------------------------------------- +% The v2 introduction should explain the structure of the paper, +% and describe the 2018 white paper process. + \include{introduction} % -------------------------------------------------------------------- -\include{cadexp2} +\part{Simulations} +\def\partname{sims}\label{part:\partname} -% -------------------------------------------------------------------- +% v2 could have two chapters, for the two suite of simulations we +% now have: -\include{solarsystem} +\include{cadexp2} +% \include{cadexp2018} % -------------------------------------------------------------------- -\include{galaxy} +\part{Science Cases and Performance Metrics} +\def\partname{science}\label{part:\partname} -% -------------------------------------------------------------------- +% The science chapters will need updating and extending with the +% 2018 white paper content. We might consider re-organizing them +% into 4 themes. +\include{solarsystem} +\include{galaxy} \include{variables} - -% -------------------------------------------------------------------- - \include{transients} - -% -------------------------------------------------------------------- - \include{magclouds} - -% -------------------------------------------------------------------- - \include{agn} - -% -------------------------------------------------------------------- - \include{cosmology} - -% -------------------------------------------------------------------- - \include{specialsurveys} +\include{wfirst} + +% The tradeoffs chapter was a summary of the v1 analysis, and will need +% updating for v2: +\include{tradeoffs} % -------------------------------------------------------------------- -\include{wfirst} +\part{Proposed Observing Strategies} +\def\partname{proposals}\label{part:\partname} -% -------------------------------------------------------------------- +% Chapters collecting together the various proposed cadences. This +% may not be the best way to do it; science theme could make more sense. +% \include{wfd} +% \include{ddf} +% \include{mini-surveys} +% \include{too} -\include{tradeoffs} +% The SAC will provide a summary of their findings and conclusions, +% including a list of new cadences to be simulated: +% \include{sac-summary} % -------------------------------------------------------------------- From 66c9330945ce171fc4f3739b2a3b72312411866f Mon Sep 17 00:00:00 2001 From: Phil Marshall Date: Sun, 18 Nov 2018 19:18:38 -0800 Subject: [PATCH 5/6] Copyright 2017 --- README.md | 2 +- 1 file changed, 1 insertion(+), 1 deletion(-) diff --git a/README.md b/README.md index 7bbdd12..6b05e50 100644 --- a/README.md +++ b/README.md @@ -55,7 +55,7 @@ End of old workshop links --> This effort is being coordinated by [Phil Marshall](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues/new?body=@drphilmarshall) (the v1 COSEP's editor-in-chief), with guidance from [Zeljko Ivezic](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues/new?body=@ivezic) and [Lynne Jones](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues/new?body=@rhiannonlynne). Any of them can propagate your privately-communicated concerns into a redacted issue on this repository. Contributions are very welcome from all round the LSST science collaborations, and beyond. Perhaps we are missing a science case? Or an idea for how to perturb the observing strategy? We'd like to hear from you! Please send all your feedback to [this repo's issues](https://github.com/LSSTScienceCollaborations/ObservingStrategy/issues). -All COSEP content is Copyright 2015, 2016, 2017, 2018 The Authors. If you make use of the ideas and results in the COSEP in your research, please cite it as **"(LSST Science Collaborations 2017)"**, and provide the URL of this repository: https://github.com/LSSTScienceCollaborations/ObservingStrategy. The BibTeX entry for the v1 COSEP is below. Thanks! +All COSEP content is Copyright 2017 The Authors. If you make use of the ideas and results in the COSEP in your research, please cite it as **"(LSST Science Collaborations 2017)"**, and provide the URL of this repository: https://github.com/LSSTScienceCollaborations/ObservingStrategy. The BibTeX entry for the v1 COSEP is below. Thanks! ``` @ARTICLE{LSST-COSEP, From 4e2c6d55c1726bef8c805f0de2ff980c3332d888 Mon Sep 17 00:00:00 2001 From: Phil Marshall Date: Sun, 18 Nov 2018 19:25:22 -0800 Subject: [PATCH 6/6] Included MS comments in the tex file to help guide implementation --- .../LSST_Observing_Strategy_White_Paper.tex | 25 +++++++++++++++---- 1 file changed, 20 insertions(+), 5 deletions(-) diff --git a/whitepaper/LSST_Observing_Strategy_White_Paper.tex b/whitepaper/LSST_Observing_Strategy_White_Paper.tex index e4c328c..d551b37 100644 --- a/whitepaper/LSST_Observing_Strategy_White_Paper.tex +++ b/whitepaper/LSST_Observing_Strategy_White_Paper.tex @@ -75,10 +75,22 @@ \part{Simulations} \def\partname{sims}\label{part:\partname} -% v2 could have two chapters, for the two suite of simulations we -% now have: - -\include{cadexp2} +% Comment from Michael Strauss: I would suggest that we not simply copy +% Chapter 2 (cadexp2) of the previous COSEP into V2, as it will just +% confuse people who want a clean story about the status of the simulations. +% The earlier version had a lot of "aspirational" words about, e.g., +% rolling cadence, that now is implementable with the feature-based scheduler, +% and I think we can tell a cleaner story without all the detours that were taken at the time V1 was written. + +% There have been lots of changesin how cadences are simulated - let's +% summarize them here: +% \include{opsim-intro} +% This section shoudl include some history, to make the work that refers +% to minion_1016 etc make sense. That history can be distilled from +% cadexp2.tex. + +% Then, we can explain the new set of simulations that was provided with +% the 2018 WP call. % \include{cadexp2018} % -------------------------------------------------------------------- @@ -117,8 +129,11 @@ \part{Proposed Observing Strategies} % \include{too} % The SAC will provide a summary of their findings and conclusions, -% including a list of new cadences to be simulated: +% including a discussion of next steps (the SAC's recommendations): % \include{sac-summary} +% Comment from Michael Strauss: This summary will also likely appear in +% a separate public document. + % --------------------------------------------------------------------