arXiv:1807.04768v2 [astro-ph.GA] 10 Jun 2019 2Jn 2019 June 12 o.Nt .Ato.Soc. Astron. R. Not. Mon. aaiaBarai Paramita Redshifts High in at Feedback Galaxies and Dwarf Growth Hole Black Intermediate-Mass lc oe Bs r sal bevdt eo stellar- of be to observed usually are ( mass (BHs) holes Black INTRODUCTION 1 ina l omcepochs, AGN emis- cosmic multi-wavelength 2005). all Ford their at & through Ferrarese sion observed 1984; widely Rees accretion are the (e.g., by the matter powered energy at of eno feedback liberate exist of which 2018). amounts (AGN), to mous nuclei al. believed galactic et active Giesers are of centers 2007; (SMBHs) globular al. BHs in et Supermassive recently 2007; Maccarone al. more (e.g., et and Orosz clusters 2016), 1983; al. al. et et galax- Cowley Corral-Santana other 1972; and Way Bolton Milky (e.g., our ies in existing binaries X-ray in 10 c u oMta 26 ˜oPuo 50-9,Brasil 05508-090, S˜ao Paulo, Mat˜ao 1226, do Rua 1 9 nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto 00RAS 0000 M ⊙ M .Selrms H aebe itrclyobserved historically been have BHs Stellar-mass ). BH ∼ 1 − 100 M 1 ⊙ lsbt .d ovi a Pino Dal Gouveia de M. Elisabete , 000 ,o uemsie( supermassive or ), z 0–0 00)Pitd1 ue21 M L (MN 2019 June 12 Printed (0000) 000–000 , 0 = ABSTRACT eetyIBshv tre ob bevda h etr flow (2 of centers of supe the simulations at and hydrodynamical observed stellar-mass be cosmological to to perform compared started have population IMBHs elusive Recently an of comprise pIBso few a of IMBHs up n netgt h rwhadfebc fcnrlIBsi dwar in IMBHs at central appear of BHs feedback earliest and The growth the investigate and ymre ihohrBs efidta,satn rm10 from starting that, find We BHs. other with merger by asv hn4 than massive M est SR)eouino h G selrms 10 mass (stellar DGs the of evolution (SFRD) density eue yfcosu o3 hnteBshv rw oafwtimes few a to grown have BHs the when 3, to up factors by reduced between ntepeec fsrne Ndie aseeto,teBscon BHs the ejection, mass SN-driven stronger of to presence the in upr h cnrota al edakfo MH ngsrc D gas-rich in IMBHs from sim feedback numerical early that on scenario based the conclusions, support Our environment. cosmological etr rwfse hnterhs aaisi h al Universe, dormant. early BHs I the words: the that Key and in DGs galaxies suggest the host results turns their feedback Our the than BH within 2017). faster range grow (Silk mass DG centers scenario the cosmological in anomalies ΛCDM several solve potentially can e:hg-esit–(aais)qaas uemsiebakhls– holes black supermassive quasars: hydrodynamics – (galaxies:) – high-redshift ies: − ˙ BH ,satn rmtelo- the from starting 7, z nemdaems lc oe IBs assbten100 between masses (IMBHs: holes black Intermediate-mass ∼ (0 = ,ssandb a nosdie yglx egr n interaction and mergers galaxy by driven inflows gas by sustained 6, z . 2 4 = M − BH csooy)lresaesrcueo nvre–glxe:daf– dwarf galaxies: – Universe of structure large-scale (cosmology:) 0 − × . 8) ∼ .Sa omto sqece between quenched is formation Star 6. 10 M 10 × cs-Uiesdd eSa al (IAG-USP), S˜ao Paulo de Universidade - icas ˙ 7 10 Edd 6 M − r- 5 ⊙ − h Haceinrtsices ihtm,adreaches and time, with increase rates accretion BH The . o h asv MH by IMBHs massive the for 10 z 6 ietclas cnro onatrteBgBn.Massive Bang. Big the the after (in soon seeds scenario) BH massive collapse the (e.g. formed direct in have accretion processes could Universe exotic enhanced early some rapid Or, by growth). grow super-Eddington could BHs SMBHs the stellar-mass scenario, one from In masses. solar of lions ac- disc thermal cold rates. a from sub-Eddington mass at on BH creting 2012; based the 2018b), al. of al. et calculation et Sutton the Mezcua 2003; 2018; al. al. et et sources Miller Caballero-Garcia X-ray (e.g., ultra-luminous IMBHs ar- in be studies BHs could Some accreting observed. the widely that as gue not however are 2018) we 100 tween 2011). 1995; al. Padovani et & Mortlock Urry 2009; (e.g., ago Alexander Gyr & 13 Goulding to up Universe cal M ∼ ⊙ 18 ed o nwhwteSBsi G rwt bil- to grew AGN in SMBHs the how know not do We nemdaems lc oe IBs fmse be- masses of (IMBHs) holes black Intermediate-mass by − z 5 n rwteefe yaceiggsand gas accreting by thereafter grow and 25, − ,we h H r eddi ao less halos in seeded are BHs the when 5, = 10 A T 1 6 E M tl l v2.2) file style X ⊙ eg,vndrMrl20;Gaa tal. et Graham 2004; Marel der van (e.g., z 5 − .Tesa omto rate formation star The 4. = h 10 2 − M z 1 8 M ⊙ 9 = Mpc) ti osbet build to possible is it , ⊙ − a ekplateau peak a has ) 10 − ms aais We galaxies. -mass 3 lc oephysics hole black iu ogo up grow to tinue n h resulting the and 6 aais(DGs). galaxies f .TeSR is SFRD The 4. sat Gs M ooigboxes comoving lto results, ulation msieBHs. rmassive Bsa DG at MBHs ⊙ 10 historically ) concordance 5 M z ⊙ 5 = Even . galax- na in s − 8 2 P. Barai et al. seed IMBHs could be a possible explanation for the origin of suming a bolometric luminosity of 10% of the Eddington) in 3 6 SMBHs. A recent study by Kovetz et al. (2018) suggest that the range 10 − 10 M⊙. gravitational wave measurements using the advanced LIGO Recently the highest-redshift discovery of AGN in DGs over six years can be used to limit the formation mecha- has been made by Mezcua et al. (2018a). They present a nism of IMBHs by the runaway merger of stellar-mass BHs sample of 40 AGN of type 2 at z 6 2.4 with luminosities 39 44 in globular clusters. in the range L0.5−10keV ∼ 10 − 10 erg/s. The hosts are 7 9 Relatively recently, massive BHs have started to be DGs with stellar masses between 10 − 3 × 10 M⊙, selected observed hosted in Dwarf Galaxies (DGs). Dynamical BH from the Chandra COSMOS-Legacy survey. Estimating the mass limits detected in nearby dwarfs include several ex- BH masses using the local scaling relation between BH and 6 amples such as: MBH ∼ 3 × 10 M⊙ in the dwarf ellipti- stellar mass (Reines & Volonteri 2015), all the AGN are con- 4 5 5 ∼ − ⊙ cal galaxy M32 (van der Marel et al. 1998); MBH ∼ 10 M⊙ sistent with hosting 10 10 M IMBHs (with a scatter in the dwarf lenticular field galaxy NGC 404 (Seth et al. of 0.55 dex), of typical Eddington ratios (or, the ratio of 4 2010); MBH < 2 × 10 M⊙ in the dwarf elliptical galaxy the BH accretion rate to the Eddington rate) > 1%. Ac- 6 NGC 205 (Valluri et al. 2005); and MBH < 10 M⊙ in the cording to Mezcua et al. (2018a), the observational trends dwarf spheroidal galaxy Ursa Minor (Demers et al. 1995). suggest that AGN in DGs evolve differently than those in more-massive galaxies. Some of the central IMBHs in DGs show signa- AGN influence the formation and evolution of galaxies tures of activity in the form of low-luminosity AGN. in the form of feedback, affecting the environment from pc NGC 4395 is a bulgeless dwarf galaxy with an ex- to Mpc scales (e.g., Silk & Rees 1998; Barai 2008; Fabian tremely faint Seyfert 1 nucleus (Filippenko & Sargent 1989), 4 2012). Supermassive BHs and host galaxies are argued to and an estimated central BH mass MBH ∼ 10 − 3 × 5 coevolve, generating observational trends such as the cen- 10 M⊙ (Peterson et al. 2005; Woo et al. 2019). Pox 52 (G tral BH mass - host galaxy stellar bulge mass correla- 1200-2038) is a dwarf galaxy with Seyfert characteristics tions (e.g., Magorrian et al. 1998; Gebhardt et al. 2000). (Kunth, Sargent & Bothun 1987), having a central BH of 5 The SMBH energy output is often observed as various forms MBH ∼ (2 − 4) × 10 M⊙ (Thornton et al. 2008). The dwarf of AGN outflows (e.g., Crenshaw, Kraemer & George 2003; starburst galaxy Henize 2-10 (Reines et al. 2011) has an Cicone et al. 2014; Melioli & de Gouveia Dal Pino 2015; actively accreting massive BH with an order-of-magnitude 6 Tombesi et al. 2015; Barai et al. 2018). mass MBH ∼ 10 M⊙. Analogous to SMBHs producing AGN feedback, the The population of DGs with observed AGN signa- IMBHs are also expected to have feedback: the energy ra- tures have been increasing (e.g., Chilingarian et al. 2018). diated by IMBHs should affect their host