X-RAY DETECTED ACTIVE GALACTIC NUCLEI IN DWARF GALAXIES AT 0 &lt; z &lt; 1

Pardo, Kris; Goulding, Andy D.; Greene, Jenny E.; Somerville, Rachel S.; Gallo, Elena; Hickox, Ryan C.; Miller, Brendan P.; Reines, Amy E.; Silverman, John D.

doi:10.3847/0004-637x/831/2/203

Cited by 110 publications

(113 citation statements)

References 89 publications

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“…A search of emission-line dwarf galaxies (10 8.5 M * 10 9.5 M e ) using BPT line diagnostics identified an AGN rate of ∼0.5% (Reines et al 2013), with an additional 0.05% of dwarf galaxies searched exhibiting narrow emission lines consistent with star formation, and, broad Hα consistent with an AGN. Similarly, an X-ray survey of z<1 dwarf galaxies reported an AGN rate of 0.6%-3% (Pardo et al 2016). Of the dwarf galaxies known to host AGN, only two exhibit nuclear radio emission that appears to originate from a black hole jet, Henize 2-10 and Mrk 709 (Reines et al 2011(Reines et al , 2014.…”

Section: Implications For Source Modelsmentioning

confidence: 99%

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

Tendulkar

Bassa

Cordes

et al. 2017

ApJL

691

775

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The precise localization of the repeating fast radio burst (FRB 121102) has provided the first unambiguous association (chance coincidence probability p3×10 −4 ) of an FRB with an optical and persistent radio counterpart. We report on optical imaging and spectroscopy of the counterpart and find that it is an extended (0 6-0 8) object displaying prominent Balmer and [O III] emission lines. Based on the spectrum and emission line ratios, we classify the counterpart as a low-metallicity, star-forming, m r′ = 25.1 AB mag dwarf galaxy at a redshift of z = 0.19273(8), corresponding to a luminosity distance of 972 Mpc. From the angular size, the redshift, and luminosity, we estimate the host galaxy to have a diameter 4 kpc and a stellar mass of M * ∼(4-7)×107 M e , assuming a mass-to-light ratio between 2 to 3 M e L e −1 . Based on the Hα flux, we estimate the star formation rate of the host to be 0.4 M e yr −1 and a substantial host dispersion measure (DM) depth 324 pc cm −3 . The net DM contribution of the host galaxy to FRB 121102 is likely to be lower than this value depending on geometrical factors. We show that the persistent radio source at FRB 121102's location reported by Marcote et al. is offset from the galaxy's center of light by ∼200 mas and the host galaxy does not show optical signatures for AGN activity. If FRB 121102 is typical of the wider FRB population and if future interferometric localizations preferentially find them in dwarf galaxies with low metallicities and prominent emission lines, they would share such a preference with long gamma-ray bursts and superluminous supernovae.

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Section: Implications For Source Modelsmentioning

confidence: 99%

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

Tendulkar

Bassa

Cordes

et al. 2017

ApJL

691

775

View full text Add to dashboard Cite

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“…The existence, masses and growth rates of massive black holes at the centres of such lowmass galaxies have been the focus of extensive study and interest (e.g. Greene & Ho 2007;Reines et al 2013;Mezcua et al 2016;Pardo et al 2016;Baldassare et al 2016Baldassare et al , 2017Hood et al 2017;Chen et al 2017). Such galaxies may provide the conditions under which the seeds of supermassive black holes can form and thus may provide local analogues that can help shed light on how supermassive black holes formed and subsequently grew in the very early (z 6) universe (e.g.…”

Section: Agn Activity In Dwarf Galaxiesmentioning

confidence: 99%

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

Aird

Coil

Georgakakis

2017

Monthly Notices of the Royal Astronomical Society

167

266

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We use deep Chandra X-ray imaging to measure the distribution of specific black hole accretion rates (L X relative to the stellar mass of the galaxy) and thus trace AGN activity within star-forming and quiescent galaxies, as a function of stellar mass (from 10 8.5 -10 11.5 M ⊙ ) and redshift (to z ∼ 4). We adopt near-infrared selected samples of galaxies from the CANDELS and UltraVISTA surveys, extract X-ray data for every galaxy, and use a flexible Bayesian method to combine these data and to measure the probability distribution function of specific black hole accretion rates, λ sBHAR . We identify a broad distribution of λ sBHAR in both starforming and quiescent galaxies-likely reflecting the stochastic nature of AGN fuelling-with a roughly power-law shape that rises toward lower λ sBHAR , a steep cutoff at λ sBHAR 0.1−1 (in Eddington equivalent units), and a turnover or flattening at λ sBHAR 10 −3 − 10 −2 . We find that the probability of a star-forming galaxy hosting a moderate λ sBHAR AGN depends on stellar mass and evolves with redshift, shifting toward higher λ sBHAR at higher redshifts. This evolution is truncated at a point corresponding to the Eddington limit, indicating black holes may self-regulate their growth at high redshifts when copious gas is available. The probability of a quiescent galaxy hosting an AGN is generally lower than that of a star-forming galaxy, shows signs of suppression at the highest stellar masses, and evolves strongly with redshift. The AGN duty cycle in high-redshift (z 2) quiescent galaxies thus reaches ∼20 per cent, comparable to the duty cycle in star-forming galaxies of equivalent stellar mass and redshift.

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“…The best evidence for IMBH in dwarf galaxies comes from x-ray (Kormendy & Ho 2013;Pardo et al 2016) as well as optical emission line studies. Active galactic nuclei are found in about 1% of dwarfs, with the x-ray luminosities well in excess of an x-ray binary contribution as predicted from the star formation rate (Baldassare et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Feedback by Massive Black Holes in Gas-rich Dwarf Galaxies

Silk¹

2017

ApJL

120

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Could there be intermediate mass black holes in essentially all old dwarf galaxies? I argue that current observations of Active Galactic Nuclei in dwarfs allow such a radical hypothesis which provides early feedback and potentially provides a unifying explanation for many if not all of the apparent dwarf galaxy anomalies, such as the abundance, core-cusp, "too big to fail", ultra-faint and baryon-fraction issues. I describe the supporting arguments, which are largely circumstantial in nature, and discuss a number of tests. There is no strong motivation for modifying the nature of cold dark matter in order to explain any of the dwarf galaxy "problems".

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X-RAY DETECTED ACTIVE GALACTIC NUCLEI IN DWARF GALAXIES AT 0 < z < 1

Cited by 110 publications

References 89 publications

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

Feedback by Massive Black Holes in Gas-rich Dwarf Galaxies

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