Dwarf Galaxies With Optical Signatures of Active Massive Black Holes

Reines, Amy E.; Greene, Jenny E.; Geha, Marla

doi:10.1088/0004-637x/775/2/116

Cited by 517 publications

(887 citation statements)

References 171 publications

(295 reference statements)

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“…The right bottom subplot shows the z = 2, 5 and 7 Magorrian relations of the Tiamat result with thick lines compared with the z ∼ 0.6 Tiamat-125-HR Magorrian relation. Observations from the local Universe are indicated with different symbols (Thornton et al 2008;Jiang et al 2011;Mathur et al 2012;Jiang et al 2013;Reines et al 2013;Scott et al 2013;Busch et al 2014;Sanghvi et al 2014;Yuan et al 2014). We see that the model predicts a similar Magorrian relation at z ∼ 0.6 compared to the local observations and we find an increasing normalization towards lower redshifts in the mass range of 10 10 M < M * < 10 12 M .…”

Section: Black Hole Propertiessupporting

confidence: 51%

Dark-ages reionization and galaxy formation simulation – X. The small contribution of quasars to reionization

Qin

Mutch

Poole

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Motivated by recent measurements of the number density of faint AGN at high redshift, we investigate the contribution of quasars to reionization by tracking the growth of central supermassive black holes in an update of the Meraxes semi-analytic model. The model is calibrated against the observed stellar mass function at z ∼ 0.6 − 7, the black hole mass function at z 0.5, the global ionizing emissivity at z ∼ 2 − 5 and the Thomson scattering optical depth. The model reproduces a Magorrian relation in agreement with observations at z < 0.5 and predicts a decreasing black hole mass towards higher redshifts at fixed total stellar mass. With the implementation of an opening angle of 80 deg for quasar radiation, corresponding to an observable fraction of ∼23.4 per cent due to obscuration by dust, the model is able to reproduce the observed quasar luminosity function at z ∼ 0.6 − 6. The stellar light from galaxies hosting faint AGN contributes a significant or dominant fraction of the UV flux. At high redshift, the model is consistent with the bright end quasar luminosity function and suggests that the recent faint z ∼ 4 AGN sample compiled by Giallongo et al. (2015) includes a significant fraction of stellar light. Direct application of this luminosity function to the calculation of AGN ionizing emissivity consequently overestimates the number of ionizing photons produced by quasars by a factor of 3 at z ∼ 6. We conclude that quasars are unlikely to make a significant contribution to reionization.

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Section: Black Hole Propertiessupporting

confidence: 51%

Dark-ages reionization and galaxy formation simulation – X. The small contribution of quasars to reionization

Qin

Mutch

Poole

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…In recent years, many studies have started looking for evidence of the presence of BHs in low-mass galaxies (with stellar mass of M ∼ 10 9 M ): evidence for accreting BHs with broad Hα line in the SDSS survey (Greene & Ho 2004Dong et al 2012), evidence for narrow-line AGN in low stellar velocity dispersions (favoring the presence of a low mass BH), or at higher redshift with stacking methods (for example, X-ray stacking up to z = 1.5 Mezcua et al 2016). Reines, Greene & Geha (2013) went further and performed the first systematic search for BHs in galaxies with stellar mass of M < 3 × 10 9 M . They found 136 dwarf galaxies harboring evidences of active BHs (photoionization signatures, broad emission lines).…”

Section: Low Redshift Analogues Of High Redshift Galaxiesmentioning

confidence: 99%

“…BHs are also observed in low-mass galaxies (Greene 2012;Reines, Greene & Geha 2013;Miller et al 2015). However we also observe galaxies without any signatures of BHs (e.g., M33, NGC 205, Gebhardt et al 2001;Valluri et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Habouzit

Volonteri²,

Dubois³

2017

Monthly Notices of the Royal Astronomical Society

245

223

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Massive black holes (BHs) inhabit local galaxies, including the Milky Way and some dwarf galaxies. BH formation, occurring at early cosmic times, must account for the properties of BHs in today's galaxies, notably why some galaxies host a BH, and others do not. We investigate the formation, distribution and growth of BH 'seeds' by using the adaptive mesh refinement code Ramses. We develop an implementation of BH formation in dense, low-metallicity environments, as advocated by models invoking the collapse of the first generation of stars, or of dense nuclear star clusters. The seed masses are computed one-by-one on-the-fly, based on the star formation rate and the stellar initial mass function. This self-consistent method to seed BHs allows us to study the distribution of BHs in a cosmological context and their evolution over cosmic time. We find that all high-mass galaxies tend to host a BH, whereas low-mass counterparts have a lower probability of hosting a BH. After the end of the epoch of BH formation, this probability is modulated by the growth of the galaxy. The simulated BHs connect to low-redshift observational samples, and span a similar range in accretion properties as Lyman-Break Analogs. The growth of BHs in low-mass galaxies is stunted by strong supernova feedback. The properties of BHs in dwarf galaxies thus remain a testbed for BH formation. Simulations with strong supernova feedback, which is able to quench BH accretion in shallow potential wells, produce galaxies and BHs in better agreement with observational constraints.

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“…Conventionally, AGN searches such as this have been performed optically, via the characteristic emission lines (e.g. Decarli et al 2007;Reines et al 2013). Here, we follow Seth et al (2008) and Gallo et al (2008) and complement this with a search for nuclear X-ray emission.…”

Section: Introductionmentioning

confidence: 99%

“…Observationally, known AGN, even low-luminosity ones, are quite rare in dwarf galaxies (Greene & Ho 2007;Gallo et al 2008), though see Reines, Greene & Geha (2013) for a recent larger sample. If we simply scale down those seen in giant early-type galaxies via a standard Magorrian-type relation, this is not perhaps surprising, as it suggests that even a reasonably bright dwarf elliptical (dE) galaxy of luminosity ∼5 × 10 7 to 5 × 10 8 L (magnitude M r ∼ −14.5 to −17) should only have an SMBH of mass ∼10 5 -10 6 M (Gallo et al 2008;Reines et al 2013). In fact, it has been suggested (e.g.…”

Section: Introductionmentioning

confidence: 99%

X-ray sources in dwarf galaxies in the Virgo cluster and the nearby field

Papadopoulou

Phillipps

Young

2016

Mon. Not. R. Astron. Soc.

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The extent to which dwarf galaxies represent essentially scaled down versions of giant galaxies is an important question with regards the formation and evolution of the galaxy population as a whole. Here, we address the specific question of whether dwarf galaxies behave like smaller versions of giants in terms of their X-ray properties. We discuss two samples of around 100 objects each, dwarfs in the Virgo cluster and dwarfs in a large Northern hemisphere area. We find nine dwarfs in each sample with Chandra detections. For the Virgo sample, these are in dwarf elliptical (or dwarf lenticular) galaxies and we assume that these are (mostly) low-mass X-ray binaries (LMXB) [some may be nuclear sources]. We find a detection rate entirely consistent with scaling down from massive ellipticals, viz. about one bright (i.e. L X > 10 38 erg s −1 ) LMXB per 5 × 10 9 M of stars. For the field sample, we find one (known) Seyfert nucleus, in a galaxy which appears to be the lowest mass dwarf with a confirmed X-ray emitting nucleus. The other detections are in star-forming dwarf irregular or blue compact dwarf galaxies and are presumably high-mass X-ray binaries (HMXB). This time, we find a very similar detection rate to that in large late-type galaxies if we scale down by star formation rate, roughly one HMXB for a rate of 0.3 M per year. Nevertheless, there does seem to be one clear difference, in that the dwarf late-type galaxies with X-ray sources appear strongly biased to very low metallicity systems.

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Dwarf Galaxies With Optical Signatures of Active Massive Black Holes

Cited by 517 publications

References 171 publications

Dark-ages reionization and galaxy formation simulation – X. The small contribution of quasars to reionization

Dark-ages reionization and galaxy formation simulation – X. The small contribution of quasars to reionization

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

X-ray sources in dwarf galaxies in the Virgo cluster and the nearby field

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