[ { "key": "ZKQ3H7EG", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/ZKQ3H7EG", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/ZKQ3H7EG", "type": "text/html" }, "up": { "href": "https://api.zotero.org/groups/2916/items/HJT3Q598", "type": "application/json" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } } }, "data": { "key": "ZKQ3H7EG", "version": 1, "parentItem": "HJT3Q598", "itemType": "attachment", "linkMode": "linked_url", "title": "2010arXiv1012.0573F", "accessDate": "2011-04-06T02:07:19Z", "url": "http://adsabs.harvard.edu/abs/2010arXiv1012.0573F", "note": "", "contentType": "", "charset": "", "tags": [], "relations": {}, "dateAdded": "2011-04-06T02:07:19Z", "dateModified": "2011-04-06T02:07:19Z" } }, { "key": "HJT3Q598", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/HJT3Q598", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/HJT3Q598", "type": "text/html" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } }, "creatorSummary": "Faucher-Giguere and Loeb", "parsedDate": "2010-12-01", "numChildren": 1 }, "data": { "key": "HJT3Q598", "version": 1, "itemType": "document", "title": "Pulsar-Black Hole Binaries in the Galactic Center", "creators": [ { "creatorType": "author", "firstName": "C. -A.", "lastName": "Faucher-Giguere" }, { "creatorType": "author", "firstName": "Abraham", "lastName": "Loeb" } ], "abstractNote": "Binaries consisting of a pulsar and a black hole (BH) are a holy grail of astrophysics, both for their significance for stellar evolution and for their potential application as probes of strong gravity. In spite of extensive surveys of our Galaxy and its system of globular clusters, no pulsar-black hole (PSR-BH) binary has been found to date. Clues as to where such systems might exist are therefore highly desirable. We show that if the central parsec around Sgr A* harbors a cluster of ~25,000 stellar BHs (as predicted by mass segregation arguments) and if it is also rich in recycled pulsar binaries (by analogy with globular clusters), then 3-body exchange interactions should produce PSR-BHs in the Galactic center. Simple estimates of the formation rate and survival time of these binaries suggest that a few PSR-BHs should be present in the central parsec today. The proposed formation mechanism makes unique predictions for the PSR-BH properties: 1) the binary would reside within ~1 pc of Sgr A*; 2) the pulsar would be recycled, with a period of ~1 to a few tens of milliseconds, and a low magnetic field B<~10^10 G; 3) the binary would have high eccentricity, e~0.8, but with a large scatter; and 4) the binary would be relatively wide, with semi-major axis a_b~0.1 - >~3 AU. The potential discovery of a PSR-BH binary therefore provides a strong motivation for deep, high-frequency radio searches for recycled pulsars toward the Galactic center.", "type": "", "date": "December 1, 2010", "publisher": "", "place": "", "DOI": "", "citationKey": "", "url": "http://adsabs.harvard.edu/abs/2010arXiv1012.0573F", "accessDate": "2011-04-06T02:07:19Z", "archive": "", "archiveLocation": "", "shortTitle": "", "language": "", "libraryCatalog": "NASA ADS", "callNumber": "", "rights": "", "extra": "", "tags": [ { "tag": "Astrophysics - High Energy Astrophysical Phenomena", "type": 1 } ], "collections": [], "relations": {}, "dateAdded": "2011-04-06T02:07:19Z", "dateModified": "2011-04-06T02:07:19Z" } }, { "key": "Q5ABWN4Q", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/Q5ABWN4Q", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/Q5ABWN4Q", "type": "text/html" }, "up": { "href": "https://api.zotero.org/groups/2916/items/ET45FNWT", "type": "application/json" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } } }, "data": { "key": "Q5ABWN4Q", "version": 1, "parentItem": "ET45FNWT", "itemType": "attachment", "linkMode": "linked_url", "title": "2011PhRvD..83f4008R", "accessDate": "2011-04-06T02:06:17Z", "url": "http://adsabs.harvard.edu/abs/2011PhRvD..83f4008R", "note": "", "contentType": "", "charset": "", "tags": [], "relations": {}, "dateAdded": "2011-04-06T02:06:17Z", "dateModified": "2011-04-06T02:06:17Z" } }, { "key": "ET45FNWT", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/ET45FNWT", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/ET45FNWT", "type": "text/html" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } }, "creatorSummary": "Reisswig et al.", "parsedDate": "2011-03-01", "numChildren": 1 }, "data": { "key": "ET45FNWT", "version": 1, "itemType": "journalArticle", "title": "Gravitational wave extraction in simulations of rotating stellar core collapse", "creators": [ { "creatorType": "author", "firstName": "C.", "lastName": "Reisswig" }, { "creatorType": "author", "firstName": "C. D.", "lastName": "Ott" }, { "creatorType": "author", "firstName": "U.", "lastName": "Sperhake" }, { "creatorType": "author", "firstName": "E.", "lastName": "Schnetter" } ], "abstractNote": "We perform simulations of general relativistic rotating stellar core collapse and compute the gravitational waves (GWs) emitted in the core-bounce phase of three representative models via multiple techniques. The simplest technique, the quadrupole formula (QF), estimates the GW content in the spacetime from the mass-quadrupole tensor only. It is strictly valid only in the weak-field and slow-motion approximation. For the first time, we apply GW extraction methods in core collapse that are fully curvature based and valid for strongly radiating and highly relativistic sources. These techniques are not restricted to weak-field and slow-motion assumptions. We employ three extraction methods computing (i) the Newman-Penrose (NP) scalar Ψ4, (ii) Regge-Wheeler-Zerilli-Moncrief master functions, and (iii) Cauchy-characteristic extraction (CCE) allowing for the extraction of GWs at future null infinity, where the spacetime is asymptotically flat and the GW content is unambiguously defined. The latter technique is the only one not suffering from residual gauge and finite-radius effects. All curvature-based methods suffer from strong nonlinear drifts. We employ the fixed-frequency integration technique as a high-pass waveform filter. Using the CCE results as a benchmark, we find that finite-radius NP extraction yields results that agree nearly perfectly in phase, but differ in amplitude by ˜1%–7% at core bounce, depending on the model. Regge-Wheeler-Zerilli-Moncrief waveforms, while, in general, agreeing in phase, contain spurious high-frequency noise of comparable amplitudes to those of the relatively weak GWs emitted in core collapse. We also find remarkably good agreement of the waveforms obtained from the QF with those obtained from CCE. The results from QF agree very well in phase and systematically underpredict peak amplitudes by ˜5%–11%, which is comparable to the NP results and is certainly within the uncertainties associated with core collapse physics.", "publicationTitle": "Physical Review D", "publisher": "", "place": "", "date": "March 1, 2011", "volume": "83", "issue": "", "section": "", "partNumber": "", "partTitle": "", "pages": "64008", "series": "", "seriesTitle": "", "seriesText": "", "journalAbbreviation": "", "DOI": "", "citationKey": "", "url": "http://adsabs.harvard.edu/abs/2011PhRvD..83f4008R", "accessDate": "2011-04-06T02:06:17Z", "PMID": "", "PMCID": "", "ISSN": "", "archive": "", "archiveLocation": "", "shortTitle": "", "language": "", "libraryCatalog": "NASA ADS", "callNumber": "", "rights": "", "extra": "", "tags": [ { "tag": "Finite-difference methods", "type": 1 }, { "tag": "Numerical relativity", "type": 1 }, { "tag": "Supernovae", "type": 1 }, { "tag": "Wave generation and sources", "type": 1 } ], "collections": [], "relations": {}, "dateAdded": "2011-04-06T02:06:17Z", "dateModified": "2011-04-06T02:06:17Z" } }, { "key": "K93M7TXR", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/K93M7TXR", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/K93M7TXR", "type": "text/html" }, "up": { "href": "https://api.zotero.org/groups/2916/items/HEXUNKS4", "type": "application/json" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } } }, "data": { "key": "K93M7TXR", "version": 1, "parentItem": "HEXUNKS4", "itemType": "attachment", "linkMode": "linked_url", "title": "2010arXiv1011.6387F", "accessDate": "2011-04-06T01:54:44Z", "url": "http://adsabs.harvard.edu/abs/2010arXiv1011.6387F", "note": "", "contentType": "", "charset": "", "tags": [], "relations": {}, "dateAdded": "2011-04-06T01:54:44Z", "dateModified": "2011-04-06T01:54:44Z" } }, { "key": "HEXUNKS4", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/HEXUNKS4", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/HEXUNKS4", "type": "text/html" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } }, "creatorSummary": "Falta et al.", "parsedDate": "2010-11-01", "numChildren": 1 }, "data": { "key": "HEXUNKS4", "version": 1, "itemType": "document", "title": "Gravitational Wave Emission from the Single-Degenerate Channel of Type Ia Supernovae", "creators": [ { "creatorType": "author", "firstName": "David", "lastName": "Falta" }, { "creatorType": "author", "firstName": "Robert T.", "lastName": "Fisher" }, { "creatorType": "author", "firstName": "Gaurav", "lastName": "Khanna" } ], "abstractNote": "The thermonuclear explosion of a C/O white dwarf as a Type Ia supernova (SN Ia) generates a kinetic energy comparable to that released by a massive star during a SN II event. Current observations and theoretical models have established that SNe Ia are asymmetric, and therefore -- like SNe II -- potential sources of gravitational wave (GW) radiation. We establish an upper-bound GW amplitude and expected frequency range based upon the energetics and nucleosynthetic yields of SNe Ia. We perform the first detailed calculations of the gravitationally-confined detonation (GCD) mechanism and first for a SN Ia of any type within the single-degenerate channel of SNe Ia. The GCD mechanism predicts a strongly-polarized GW burst from the SD channel of SNe Ia in the frequency band around 1 Hz. Third-generation spaceborne GW observatories currently in planning, including the Big Bang Observer (BBO), and the Deci-Hertz Interferometer Gravitational Wave Observatory (DECIGO), as well as earthbound instruments, including the Einstein Telescope (ET), may be able to detect the signal predicted by the GCD mechanism from galactic SNe Ia and nearby extragalactic SNe Ia at distances up to 1 Mpc. If observable, GWs may offer a direct probe into the first few seconds of SNe Ia, and yield insights into its underlying detonation mechanism not possible in the optical portion of the spectrum.", "type": "", "date": "November 1, 2010", "publisher": "", "place": "", "DOI": "", "citationKey": "", "url": "http://adsabs.harvard.edu/abs/2010arXiv1011.6387F", "accessDate": "2011-04-06T01:54:44Z", "archive": "", "archiveLocation": "", "shortTitle": "", "language": "", "libraryCatalog": "NASA ADS", "callNumber": "", "rights": "", "extra": "", "tags": [ { "tag": "Astrophysics - High Energy Astrophysical Phenomena", "type": 1 }, { "tag": "General Relativity and Quantum Cosmology", "type": 1 } ], "collections": [], "relations": {}, "dateAdded": "2011-04-06T01:54:44Z", "dateModified": "2011-04-06T01:54:44Z" } }, { "key": "R5QK6GUH", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/R5QK6GUH", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/R5QK6GUH", "type": "text/html" }, "up": { "href": "https://api.zotero.org/groups/2916/items/3V6BUBK3", "type": "application/json" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } } }, "data": { "key": "R5QK6GUH", "version": 1, "parentItem": "3V6BUBK3", "itemType": "attachment", "linkMode": "linked_url", "title": "2010arXiv1011.5909K", "accessDate": "2011-04-06T01:26:35Z", "url": "http://adsabs.harvard.edu/abs/2010arXiv1011.5909K", "note": "", "contentType": "", "charset": "", "tags": [], "relations": {}, "dateAdded": "2011-04-06T01:26:35Z", "dateModified": "2011-04-06T01:26:35Z" } }, { "key": "3V6BUBK3", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/3V6BUBK3", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/3V6BUBK3", "type": "text/html" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } }, "creatorSummary": "Khoury", "parsedDate": "2010-11-01", "numChildren": 1 }, "data": { "key": "3V6BUBK3", "version": 1, "itemType": "document", "title": "Theories of Dark Energy with Screening Mechanisms", "creators": [ { "creatorType": "author", "firstName": "Justin", "lastName": "Khoury" } ], "abstractNote": "Despite the overwhelming evidence for the existence of dark energy and dark matter, their underlying fundamental physics remains unknown. This review article explores the tantalizing possibility that the dark sector includes new light degrees of freedom that mediate long-range forces on cosmological scales. To ensure consistency with laboratory and solar system tests of gravity, some screening mechanism is necessary to \"hide\" these degrees of freedom locally. I will focus on two broad classes of screening theories, chameleons and symmetrons, which rely respectively on the scalar field acquiring a large mass or weak coupling in the presence of large ambient matter density.", "type": "", "date": "November 1, 2010", "publisher": "", "place": "", "DOI": "", "citationKey": "", "url": "http://adsabs.harvard.edu/abs/2010arXiv1011.5909K", "accessDate": "2011-04-06T01:26:35Z", "archive": "", "archiveLocation": "", "shortTitle": "", "language": "", "libraryCatalog": "NASA ADS", "callNumber": "", "rights": "", "extra": "", "tags": [ { "tag": "Astrophysics - Cosmology and Extragalactic Astrophysics", "type": 1 }, { "tag": "High Energy Physics - Theory", "type": 1 } ], "collections": [], "relations": {}, "dateAdded": "2011-04-06T01:26:35Z", "dateModified": "2011-04-06T01:26:35Z" } }, { "key": "QCFTC7BJ", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/QCFTC7BJ", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/QCFTC7BJ", "type": "text/html" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } }, "creatorSummary": "Sesana et al.", "parsedDate": "2011-02-01", "numChildren": 1 }, "data": { "key": "QCFTC7BJ", "version": 1, "itemType": "journalArticle", "title": "Reconstructing the massive black hole cosmic history through gravitational waves", "creators": [ { "creatorType": "author", "firstName": "Alberto", "lastName": "Sesana" }, { "creatorType": "author", "firstName": "Jonathan", "lastName": "Gair" }, { "creatorType": "author", "firstName": "Emanuele", "lastName": "Berti" }, { "creatorType": "author", "firstName": "Marta", "lastName": "Volonteri" } ], "abstractNote": "The massive black holes we observe in galaxies today are the natural end-product of a complex evolutionary path, in which black holes seeded in proto-galaxies at high redshift grow through cosmic history via a sequence of mergers and accretion episodes. Electromagnetic observations probe a small subset of the population of massive black holes (namely, those that are active or those that are very close to us), but planned space-based gravitational wave observatories such as the Laser Interferometer Space Antenna (LISA) can measure the parameters of “electromagnetically invisible” massive black holes out to high redshift. In this paper we introduce a Bayesian framework to analyze the information that can be gathered from a set of such measurements. Our goal is to connect a set of massive black hole binary merger observations to the underlying model of massive black hole formation. In other words, given a set of observed massive black hole coalescences, we assess what information can be extracted about the underlying massive black hole population model. For concreteness we consider ten specific models of massive black hole formation, chosen to probe four important (and largely unconstrained) aspects of the input physics used in structure formation simulations: seed formation, metallicity “feedback”, accretion efficiency and accretion geometry. For the first time we allow for the possibility of “model mixing”, by drawing the observed population from some combination of the “pure” models that have been simulated. A Bayesian analysis allows us to recover a posterior probability distribution for the “mixing parameters” that characterize the fractions of each model represented in the observed distribution. Our work shows that LISA has enormous potential to probe the underlying physics of structure formation.", "publicationTitle": "Physical Review D", "publisher": "", "place": "", "date": "February 1, 2011", "volume": "83", "issue": "", "section": "", "partNumber": "", "partTitle": "", "pages": "44036", "series": "", "seriesTitle": "", "seriesText": "", "journalAbbreviation": "", "DOI": "", "citationKey": "", "url": "http://adsabs.harvard.edu/abs/2011PhRvD..83d4036S", "accessDate": "2011-04-06T01:23:57Z", "PMID": "", "PMCID": "", "ISSN": "", "archive": "", "archiveLocation": "", "shortTitle": "", "language": "", "libraryCatalog": "NASA ADS", "callNumber": "", "rights": "", "extra": "", "tags": [ { "tag": "Black holes", "type": 1 }, { "tag": "Gravitational waves: theory", "type": 1 }, { "tag": "Gravitational-wave astrophysics", "type": 1 }, { "tag": "Physics of black holes", "type": 1 } ], "collections": [], "relations": {}, "dateAdded": "2011-04-06T01:23:57Z", "dateModified": "2011-04-06T01:23:57Z" } }, { "key": "6M4E2RMV", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/6M4E2RMV", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/6M4E2RMV", "type": "text/html" }, "up": { "href": "https://api.zotero.org/groups/2916/items/QCFTC7BJ", "type": "application/json" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } } }, "data": { "key": "6M4E2RMV", "version": 1, "parentItem": "QCFTC7BJ", "itemType": "attachment", "linkMode": "linked_url", "title": "2011PhRvD..83d4036S", "accessDate": "2011-04-06T01:23:57Z", "url": "http://adsabs.harvard.edu/abs/2011PhRvD..83d4036S", "note": "", "contentType": "", "charset": "", "tags": [], "relations": {}, "dateAdded": "2011-04-06T01:23:57Z", "dateModified": "2011-04-06T01:23:57Z" } }, { "key": "WVA25ZII", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/WVA25ZII", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/WVA25ZII", "type": "text/html" }, "up": { "href": "https://api.zotero.org/groups/2916/items/CWJISTNM", "type": "application/json" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } } }, "data": { "key": "WVA25ZII", "version": 1, "parentItem": "CWJISTNM", "itemType": "attachment", "linkMode": "linked_url", "title": "2010AIPC.1314..217W", "accessDate": "2011-04-06T01:21:52Z", "url": "http://adsabs.harvard.edu/abs/2010AIPC.1314..217W", "note": "", "contentType": "", "charset": "", "tags": [], "relations": {}, "dateAdded": "2011-04-06T01:21:52Z", "dateModified": "2011-04-06T01:21:52Z" } }, { "key": "CWJISTNM", "version": 1, "library": { "type": "group", "id": 2916, "name": "Favata's ''Best'' of the arXiv", "links": { "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv", "type": "text/html" } } }, "links": { "self": { "href": "https://api.zotero.org/groups/2916/items/CWJISTNM", "type": "application/json" }, "alternate": { "href": "https://www.zotero.org/groups/favatas_best_of_the_arxiv/items/CWJISTNM", "type": "text/html" } }, "meta": { "createdByUser": { "id": 34186, "username": "favata", "name": "Marc Favata", "links": { "alternate": { "href": "https://www.zotero.org/favata", "type": "text/html" } } }, "creatorSummary": "Webbink", "parsedDate": "2010-12-01", "numChildren": 1 }, "data": { "key": "CWJISTNM", "version": 1, "itemType": "conferencePaper", "title": "Watch This Space: Observing Merging White Dwarfs", "creators": [ { "creatorType": "author", "firstName": "Ronald F.", "lastName": "Webbink" } ], "abstractNote": "The Laser Interferometer Space Antenna (LISA) will open the low-frequency (0.1-100 mHz) part of the gravitational wave spectrum to direct observation. Of order 3600 galactic close binary white dwarfs will be individually resolvable in its all-sky spectrum, of which a dozen systems are expected to be on the verge of merger, showing the effects of strong tidal heating and/or early onset of tidal mass transfer. Optical study of these systems would provide important insights into tidal dissipation mechanisms, and internal heating in merging white dwarfs that sets ignition conditions for potential type Ia super-novae. 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H.", "lastName": "Suyu" }, { "creatorType": "author", "firstName": "A.", "lastName": "Halkola" } ], "abstractNote": "Strong gravitational lensing by groups or clusters of galaxies provides a powerful technique to measure the dark matter properties of individual lens galaxies. We study in detail the mass distribution of the satellite lens galaxy in the group-scale lens SL2S J08544-0121 by modelling simultaneously the spatially extended surface brightness distribution of the source galaxy and the lens mass distribution using Markov chain Monte Carlo methods. In particular, we measure the dark matter halo size of the satellite lens galaxy to be 6.0+2.9-2.0 kpc with a fiducial velocity dispersion of 127+21-12 km s-1. This is the first time the size of an individual galaxy halo in a galaxy group has been measured using strong gravitational lensing without assumptions of mass following light. We verify the robustness of our halo size measurement using mock data resembling our lens system. Our measurement of the halo size is compatible with the estimated tidal radius of the satellite galaxy, suggesting that halos of galaxies in groups experience significant tidal stripping, a process that has been previously observed on galaxies in clusters. Our mass model of the satellite galaxy is elliptical with its major axis misaligned with that of the light by ~50°. The major axis of the total matter distribution is oriented more towards the centre of the host halo, exhibiting the radial alignment found in N-body simulations and observational studies of satellite galaxies. This misalignment between mass and light poses a significant challenge to modified Newtonian dynamics. Based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. 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