Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies

We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Michael S. Fusco [verfasserIn] Benjamin L. Davis [verfasserIn] Julia Kennefick [verfasserIn] Daniel Kennefick [verfasserIn] Marc S. Seigar [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2022

Schlagwörter:	black hole physics galaxies: spiral galaxies: structure galaxies: statistics

Übergeordnetes Werk:	In: Universe - MDPI AG, 2015, 8(2022), 12, p 649
Übergeordnetes Werk:	volume:8 ; year:2022 ; number:12, p 649

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3390/universe8120649

Katalog-ID:	DOAJ082960151

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520			\|a We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors.
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author_variant	m s f msf b l d bld j k jk d k dk m s s mss
matchkey_str	article:22181997:2022----::rbnteomsedfhbakoeasuciniatdofi
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publishDate	2022
allfields	10.3390/universe8120649 doi (DE-627)DOAJ082960151 (DE-599)DOAJf9c68a8939a24f23959be67b6e8624a2 DE-627 ger DE-627 rakwb eng QC793-793.5 Michael S. Fusco verfasserin aut Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors. black hole physics galaxies: spiral galaxies: structure galaxies: statistics Elementary particle physics Benjamin L. Davis verfasserin aut Julia Kennefick verfasserin aut Daniel Kennefick verfasserin aut Marc S. Seigar verfasserin aut In Universe MDPI AG, 2015 8(2022), 12, p 649 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:12, p 649 https://doi.org/10.3390/universe8120649 kostenfrei https://doaj.org/article/f9c68a8939a24f23959be67b6e8624a2 kostenfrei https://www.mdpi.com/2218-1997/8/12/649 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 8 2022 12, p 649
spelling	10.3390/universe8120649 doi (DE-627)DOAJ082960151 (DE-599)DOAJf9c68a8939a24f23959be67b6e8624a2 DE-627 ger DE-627 rakwb eng QC793-793.5 Michael S. Fusco verfasserin aut Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors. black hole physics galaxies: spiral galaxies: structure galaxies: statistics Elementary particle physics Benjamin L. Davis verfasserin aut Julia Kennefick verfasserin aut Daniel Kennefick verfasserin aut Marc S. Seigar verfasserin aut In Universe MDPI AG, 2015 8(2022), 12, p 649 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:12, p 649 https://doi.org/10.3390/universe8120649 kostenfrei https://doaj.org/article/f9c68a8939a24f23959be67b6e8624a2 kostenfrei https://www.mdpi.com/2218-1997/8/12/649 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 8 2022 12, p 649
allfields_unstemmed	10.3390/universe8120649 doi (DE-627)DOAJ082960151 (DE-599)DOAJf9c68a8939a24f23959be67b6e8624a2 DE-627 ger DE-627 rakwb eng QC793-793.5 Michael S. Fusco verfasserin aut Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors. black hole physics galaxies: spiral galaxies: structure galaxies: statistics Elementary particle physics Benjamin L. Davis verfasserin aut Julia Kennefick verfasserin aut Daniel Kennefick verfasserin aut Marc S. Seigar verfasserin aut In Universe MDPI AG, 2015 8(2022), 12, p 649 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:12, p 649 https://doi.org/10.3390/universe8120649 kostenfrei https://doaj.org/article/f9c68a8939a24f23959be67b6e8624a2 kostenfrei https://www.mdpi.com/2218-1997/8/12/649 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 8 2022 12, p 649
allfieldsGer	10.3390/universe8120649 doi (DE-627)DOAJ082960151 (DE-599)DOAJf9c68a8939a24f23959be67b6e8624a2 DE-627 ger DE-627 rakwb eng QC793-793.5 Michael S. Fusco verfasserin aut Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors. black hole physics galaxies: spiral galaxies: structure galaxies: statistics Elementary particle physics Benjamin L. Davis verfasserin aut Julia Kennefick verfasserin aut Daniel Kennefick verfasserin aut Marc S. Seigar verfasserin aut In Universe MDPI AG, 2015 8(2022), 12, p 649 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:12, p 649 https://doi.org/10.3390/universe8120649 kostenfrei https://doaj.org/article/f9c68a8939a24f23959be67b6e8624a2 kostenfrei https://www.mdpi.com/2218-1997/8/12/649 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 8 2022 12, p 649
allfieldsSound	10.3390/universe8120649 doi (DE-627)DOAJ082960151 (DE-599)DOAJf9c68a8939a24f23959be67b6e8624a2 DE-627 ger DE-627 rakwb eng QC793-793.5 Michael S. Fusco verfasserin aut Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors. black hole physics galaxies: spiral galaxies: structure galaxies: statistics Elementary particle physics Benjamin L. Davis verfasserin aut Julia Kennefick verfasserin aut Daniel Kennefick verfasserin aut Marc S. Seigar verfasserin aut In Universe MDPI AG, 2015 8(2022), 12, p 649 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:12, p 649 https://doi.org/10.3390/universe8120649 kostenfrei https://doaj.org/article/f9c68a8939a24f23959be67b6e8624a2 kostenfrei https://www.mdpi.com/2218-1997/8/12/649 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 8 2022 12, p 649
language	English
source	In Universe 8(2022), 12, p 649 volume:8 year:2022 number:12, p 649
sourceStr	In Universe 8(2022), 12, p 649 volume:8 year:2022 number:12, p 649
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	black hole physics galaxies: spiral galaxies: structure galaxies: statistics Elementary particle physics
isfreeaccess_bool	true
container_title	Universe
authorswithroles_txt_mv	Michael S. Fusco @@aut@@ Benjamin L. Davis @@aut@@ Julia Kennefick @@aut@@ Daniel Kennefick @@aut@@ Marc S. Seigar @@aut@@
publishDateDaySort_date	2022-01-01T00:00:00Z
hierarchy_top_id	820684236
id	DOAJ082960151
language_de	englisch
fullrecord	<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">DOAJ082960151</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20240414145615.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">230311s2022 xx \|\|\|\|\|o 00\| \|\|eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.3390/universe8120649</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)DOAJ082960151</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)DOAJf9c68a8939a24f23959be67b6e8624a2</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">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="050" ind1=" " ind2="0"><subfield code="a">QC793-793.5</subfield></datafield><datafield tag="100" ind1="0" ind2=" "><subfield code="a">Michael S. Fusco</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2022</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="520" ind1=" " ind2=" "><subfield code="a">We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). 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callnumber-first	Q - Science
author	Michael S. Fusco
spellingShingle	Michael S. Fusco misc QC793-793.5 misc black hole physics misc galaxies: spiral misc galaxies: structure misc galaxies: statistics misc Elementary particle physics Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies
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topic_title	QC793-793.5 Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies black hole physics galaxies: spiral galaxies: structure galaxies: statistics
topic	misc QC793-793.5 misc black hole physics misc galaxies: spiral misc galaxies: structure misc galaxies: statistics misc Elementary particle physics
topic_unstemmed	misc QC793-793.5 misc black hole physics misc galaxies: spiral misc galaxies: structure misc galaxies: statistics misc Elementary particle physics
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title	Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies
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title_full	Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies
author_sort	Michael S. Fusco
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author_browse	Michael S. Fusco Benjamin L. Davis Julia Kennefick Daniel Kennefick Marc S. Seigar
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title_sort	probing the low-mass end of the black hole mass function via a study of faint local spiral galaxies
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title_auth	Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies
abstract	We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors.
abstractGer	We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors.
abstract_unstemmed	We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors.
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title_short	Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies
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Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute <i<B</i<-band magnitude <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<<</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag and luminosity distance <inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<D</mi<<mi mathvariant="normal"<L</mi<</msub<<mo<≤</mo<<mn<25.4</mn<</mrow<</semantics<</math<</inline-formula< Mpc, which is an extension of a complementary set of 140 more luminous (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi mathvariant="fraktur"<M</mi<<mi<B</mi<</msub<<mo<≤</mo<<mo<−</mo<<mn<19.12</mn<</mrow<</semantics<</math<</inline-formula< mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that may hold important implications for spiral formation theories. Our data show a distinct bimodal population manifest in the pitch angles of the Sa–Sc types and separately the Scd–Sm types, with Sa–Sc types having tighter spiral arms on average. Importantly, we uncover a distinct bifurcation of the BHMF, such that the Sa–Sc galaxies typically host so-called “supermassive” black holes (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≳</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<), whereas Scd–Sm galaxies accordingly harbor black holes that are “less-than-supermassive” (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<mrow<<msub<<mi<M</mi<<mo<•</mo<</msub<<mo<≲</mo<<msup<<mn<10</mn<<mn<6</mn<</msup<<mspace width="0.166667em"<</mspace<<msub<<mi mathvariant="normal"<M</mi<<mo<⊙</mo<</msub<</mrow<</semantics<</math<</inline-formula<). It is amongst this latter population of galaxies where we expect fruitful bounties of elusive intermediate-mass black holes (IMBHs), through which a better understanding will help form more precise benchmarks for future generations of gravitational wave detectors.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">black hole physics</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">galaxies: spiral</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">galaxies: structure</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">galaxies: statistics</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Elementary particle physics</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Benjamin L. 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Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies

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