Formation of the largest galactic cores through binary scouring and gravitational wave recoil

Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic...
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Autor*in:	Nasim, Imran Tariq [verfasserIn] Gualandris, Alessia [verfasserIn] Read, Justin I [verfasserIn] Antonini, Fabio [verfasserIn] Dehnen, Walter [verfasserIn] Delorme, Maxime [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2021 February 15

Anmerkung:	Gesehen am 26.05.2021
Umfang:	21

Übergeordnetes Werk:	Enthalten in: Monthly notices of the Royal Astronomical Society - Royal Astronomical Society, Oxford : Oxford Univ. Press, 1827, 502(2021), 4 vom: Apr., Seite 4794-4814
Übergeordnetes Werk:	volume:502 ; year:2021 ; number:4 ; month:04 ; pages:4794-4814 ; extent:21

Links:	Volltext Volltext

DOI / URN:	10.1093/mnras/stab435

Katalog-ID:	1758741120

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520			\|a Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. We show that the bright ‘knots’ observed in the core region of A2261-BCG are best explained as stalled perturbers resulting from minor mergers, though the brightest may also represent ejected SMBHs surrounded by a stellar cloak of bound stars.
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allfields	10.1093/mnras/stab435 doi (DE-627)1758741120 (DE-599)KXP1758741120 (OCoLC)1341413782 DE-627 ger DE-627 rda eng Nasim, Imran Tariq verfasserin (DE-588)1234068516 (DE-627)1758741880 aut Formation of the largest galactic cores through binary scouring and gravitational wave recoil Imran Tariq Nasim, Alessia Gualandris, Justin I. Read, Fabio Antonini, Walter Dehnen and Maxime Delorme 2021 February 15 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 26.05.2021 Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. We show that the bright ‘knots’ observed in the core region of A2261-BCG are best explained as stalled perturbers resulting from minor mergers, though the brightest may also represent ejected SMBHs surrounded by a stellar cloak of bound stars. Gualandris, Alessia verfasserin aut Read, Justin I verfasserin aut Antonini, Fabio verfasserin aut Dehnen, Walter verfasserin (DE-588)1194488994 (DE-627)167650396X aut Delorme, Maxime verfasserin aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 502(2021), 4 vom: Apr., Seite 4794-4814 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:502 year:2021 number:4 month:04 pages:4794-4814 extent:21 https://doi.org/10.1093/mnras/stab435 Verlag Resolving-System lizenzpflichtig Volltext https://academic.oup.com/mnras/article/502/4/4794/6136268 Verlag lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_2810 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 502 2021 4 4 4794-4814 21 2013 01 DE-16-250 393112875X 00 --%%-- --%%-- --%%-- --%%-- l01 26-05-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_6 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1758741295 Dehnen, Walter 2013 01 DE-16-250 04 k (DE-627)1416733728 ZAH Astronomisches Recheninstitut 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_5
spelling	10.1093/mnras/stab435 doi (DE-627)1758741120 (DE-599)KXP1758741120 (OCoLC)1341413782 DE-627 ger DE-627 rda eng Nasim, Imran Tariq verfasserin (DE-588)1234068516 (DE-627)1758741880 aut Formation of the largest galactic cores through binary scouring and gravitational wave recoil Imran Tariq Nasim, Alessia Gualandris, Justin I. Read, Fabio Antonini, Walter Dehnen and Maxime Delorme 2021 February 15 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 26.05.2021 Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. We show that the bright ‘knots’ observed in the core region of A2261-BCG are best explained as stalled perturbers resulting from minor mergers, though the brightest may also represent ejected SMBHs surrounded by a stellar cloak of bound stars. Gualandris, Alessia verfasserin aut Read, Justin I verfasserin aut Antonini, Fabio verfasserin aut Dehnen, Walter verfasserin (DE-588)1194488994 (DE-627)167650396X aut Delorme, Maxime verfasserin aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 502(2021), 4 vom: Apr., Seite 4794-4814 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:502 year:2021 number:4 month:04 pages:4794-4814 extent:21 https://doi.org/10.1093/mnras/stab435 Verlag Resolving-System lizenzpflichtig Volltext https://academic.oup.com/mnras/article/502/4/4794/6136268 Verlag lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_2810 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 502 2021 4 4 4794-4814 21 2013 01 DE-16-250 393112875X 00 --%%-- --%%-- --%%-- --%%-- l01 26-05-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_6 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1758741295 Dehnen, Walter 2013 01 DE-16-250 04 k (DE-627)1416733728 ZAH Astronomisches Recheninstitut 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_5
allfields_unstemmed	10.1093/mnras/stab435 doi (DE-627)1758741120 (DE-599)KXP1758741120 (OCoLC)1341413782 DE-627 ger DE-627 rda eng Nasim, Imran Tariq verfasserin (DE-588)1234068516 (DE-627)1758741880 aut Formation of the largest galactic cores through binary scouring and gravitational wave recoil Imran Tariq Nasim, Alessia Gualandris, Justin I. Read, Fabio Antonini, Walter Dehnen and Maxime Delorme 2021 February 15 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 26.05.2021 Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. We show that the bright ‘knots’ observed in the core region of A2261-BCG are best explained as stalled perturbers resulting from minor mergers, though the brightest may also represent ejected SMBHs surrounded by a stellar cloak of bound stars. Gualandris, Alessia verfasserin aut Read, Justin I verfasserin aut Antonini, Fabio verfasserin aut Dehnen, Walter verfasserin (DE-588)1194488994 (DE-627)167650396X aut Delorme, Maxime verfasserin aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 502(2021), 4 vom: Apr., Seite 4794-4814 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:502 year:2021 number:4 month:04 pages:4794-4814 extent:21 https://doi.org/10.1093/mnras/stab435 Verlag Resolving-System lizenzpflichtig Volltext https://academic.oup.com/mnras/article/502/4/4794/6136268 Verlag lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_2810 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 502 2021 4 4 4794-4814 21 2013 01 DE-16-250 393112875X 00 --%%-- --%%-- --%%-- --%%-- l01 26-05-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_6 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1758741295 Dehnen, Walter 2013 01 DE-16-250 04 k (DE-627)1416733728 ZAH Astronomisches Recheninstitut 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_5
allfieldsGer	10.1093/mnras/stab435 doi (DE-627)1758741120 (DE-599)KXP1758741120 (OCoLC)1341413782 DE-627 ger DE-627 rda eng Nasim, Imran Tariq verfasserin (DE-588)1234068516 (DE-627)1758741880 aut Formation of the largest galactic cores through binary scouring and gravitational wave recoil Imran Tariq Nasim, Alessia Gualandris, Justin I. Read, Fabio Antonini, Walter Dehnen and Maxime Delorme 2021 February 15 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 26.05.2021 Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. We show that the bright ‘knots’ observed in the core region of A2261-BCG are best explained as stalled perturbers resulting from minor mergers, though the brightest may also represent ejected SMBHs surrounded by a stellar cloak of bound stars. Gualandris, Alessia verfasserin aut Read, Justin I verfasserin aut Antonini, Fabio verfasserin aut Dehnen, Walter verfasserin (DE-588)1194488994 (DE-627)167650396X aut Delorme, Maxime verfasserin aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 502(2021), 4 vom: Apr., Seite 4794-4814 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:502 year:2021 number:4 month:04 pages:4794-4814 extent:21 https://doi.org/10.1093/mnras/stab435 Verlag Resolving-System lizenzpflichtig Volltext https://academic.oup.com/mnras/article/502/4/4794/6136268 Verlag lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_2810 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 502 2021 4 4 4794-4814 21 2013 01 DE-16-250 393112875X 00 --%%-- --%%-- --%%-- --%%-- l01 26-05-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_6 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1758741295 Dehnen, Walter 2013 01 DE-16-250 04 k (DE-627)1416733728 ZAH Astronomisches Recheninstitut 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_5
allfieldsSound	10.1093/mnras/stab435 doi (DE-627)1758741120 (DE-599)KXP1758741120 (OCoLC)1341413782 DE-627 ger DE-627 rda eng Nasim, Imran Tariq verfasserin (DE-588)1234068516 (DE-627)1758741880 aut Formation of the largest galactic cores through binary scouring and gravitational wave recoil Imran Tariq Nasim, Alessia Gualandris, Justin I. Read, Fabio Antonini, Walter Dehnen and Maxime Delorme 2021 February 15 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 26.05.2021 Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. We show that the bright ‘knots’ observed in the core region of A2261-BCG are best explained as stalled perturbers resulting from minor mergers, though the brightest may also represent ejected SMBHs surrounded by a stellar cloak of bound stars. Gualandris, Alessia verfasserin aut Read, Justin I verfasserin aut Antonini, Fabio verfasserin aut Dehnen, Walter verfasserin (DE-588)1194488994 (DE-627)167650396X aut Delorme, Maxime verfasserin aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 502(2021), 4 vom: Apr., Seite 4794-4814 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:502 year:2021 number:4 month:04 pages:4794-4814 extent:21 https://doi.org/10.1093/mnras/stab435 Verlag Resolving-System lizenzpflichtig Volltext https://academic.oup.com/mnras/article/502/4/4794/6136268 Verlag lizenzpflichtig Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_2810 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 502 2021 4 4 4794-4814 21 2013 01 DE-16-250 393112875X 00 --%%-- --%%-- --%%-- --%%-- l01 26-05-21 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_6 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1758741295 Dehnen, Walter 2013 01 DE-16-250 04 k (DE-627)1416733728 ZAH Astronomisches Recheninstitut 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_5
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source	Enthalten in Monthly notices of the Royal Astronomical Society 502(2021), 4 vom: Apr., Seite 4794-4814 volume:502 year:2021 number:4 month:04 pages:4794-4814 extent:21
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authorswithroles_txt_mv	Nasim, Imran Tariq @@aut@@ Gualandris, Alessia @@aut@@ Read, Justin I @@aut@@ Antonini, Fabio @@aut@@ Dehnen, Walter @@aut@@ Delorme, Maxime @@aut@@
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title	Formation of the largest galactic cores through binary scouring and gravitational wave recoil
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title_full	Formation of the largest galactic cores through binary scouring and gravitational wave recoil Imran Tariq Nasim, Alessia Gualandris, Justin I. Read, Fabio Antonini, Walter Dehnen and Maxime Delorme
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title_sort	formation of the largest galactic cores through binary scouring and gravitational wave recoil
title_auth	Formation of the largest galactic cores through binary scouring and gravitational wave recoil
abstract	Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. We show that the bright ‘knots’ observed in the core region of A2261-BCG are best explained as stalled perturbers resulting from minor mergers, though the brightest may also represent ejected SMBHs surrounded by a stellar cloak of bound stars. Gesehen am 26.05.2021
abstractGer	Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. We show that the bright ‘knots’ observed in the core region of A2261-BCG are best explained as stalled perturbers resulting from minor mergers, though the brightest may also represent ejected SMBHs surrounded by a stellar cloak of bound stars. Gesehen am 26.05.2021
abstract_unstemmed	Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. We show that the bright ‘knots’ observed in the core region of A2261-BCG are best explained as stalled perturbers resulting from minor mergers, though the brightest may also represent ejected SMBHs surrounded by a stellar cloak of bound stars. Gesehen am 26.05.2021
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title_short	Formation of the largest galactic cores through binary scouring and gravitational wave recoil
url	https://doi.org/10.1093/mnras/stab435 https://academic.oup.com/mnras/article/502/4/4794/6136268
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up_date	2024-07-05T00:22:26.141Z
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fullrecord_marcxml	<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a2200265 4500</leader><controlfield tag="001">1758741120</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20220819214022.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">210526s2021 xx \|\|\|\|\|o 00\| \|\|eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1093/mnras/stab435</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)1758741120</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)KXP1758741120</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(OCoLC)1341413782</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rda</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Nasim, Imran Tariq</subfield><subfield code="e">verfasserin</subfield><subfield code="0">(DE-588)1234068516</subfield><subfield code="0">(DE-627)1758741880</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Formation of the largest galactic cores through binary scouring and gravitational wave recoil</subfield><subfield code="c">Imran Tariq Nasim, Alessia Gualandris, Justin I. Read, Fabio Antonini, Walter Dehnen and Maxime Delorme</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2021 February 15</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">21</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">Gesehen am 26.05.2021</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Massive elliptical galaxies are typically observed to have central cores in their projected radial light profiles. Such cores have long been thought to form through ‘binary scouring’ as supermassive black holes (SMBHs), brought in through mergers, form a hard binary and eject stars from the galactic centre. However, the most massive cores, like the $\sim 3{\, \mathrm{kpc}}$ core in A2261-BCG, remain challenging to explain in this way. In this paper, we run a suite of dry galaxy merger simulations to explore three different scenarios for central core formation in massive elliptical galaxies: ‘binary scouring’, ‘tidal deposition’, and ‘gravitational wave (GW) induced recoil’. Using the griffin code, we self-consistently model the stars, dark matter, and SMBHs in our merging galaxies, following the SMBH dynamics through to the formation of a hard binary. We find that we can only explain the large surface brightness core of A2261-BCG with a combination of a major merger that produces a small $\sim 1{\, \mathrm{kpc}}$ core through binary scouring, followed by the subsequent GW recoil of its SMBH that acts to grow the core size. Key predictions of this scenario are an offset SMBH surrounded by a compact cluster of bound stars and a non-divergent central density profile. 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Formation of the largest galactic cores through binary scouring and gravitational wave recoil

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