(LBT-SONG): the Satellite Population of NGC 628
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MNRAS 000,1{18 (2020) Preprint 17 September 2020 Compiled using MNRAS LATEX style file v3.0 The LBT Satellites of Nearby Galaxies Survey (LBT-SONG): The Satellite Population of NGC 628 A. Bianca Davis1;3?, Anna M. Nierenberg,4;5, Annika H. G. Peter1;2;3, Christopher T. Garling2;3, Johnny P. Greco1;3;7, Christopher S. Kochanek2;3, Dyas Utomo2, Kirsten Casey1;3, Richard W. Pogge2;3, Daniella Roberts1;3, David J. Sand6, Amy Sardone2;3;7 1Department of Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus OH 43210, USA 2Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus OH 43210, USA 3Center for Cosmology and Astroparticle Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus OH 43210, USA 4Jet Propulsion Laboratory, California Institute of Technology 5NASA Postdoctoral Program Fellow 6Steward Observatory, University of Arizona, 933 North Cherry Avenue, Rm. N204, Tucson, AZ 85721-0065, USA 7NSF Astronomy and Astrophysics Postdoctoral Fellow Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We present the first satellite system of the Large Binocular Telescope Satellites Of Nearby Galaxies Survey (LBT-SONG), a survey to characterize the close satellite populations of Large Magellanic Cloud to Milky Way-mass, star-forming galaxies in the Local Volume. In this paper, we describe our unresolved diffuse satellite finding and completeness measurement methodology and apply this framework to NGC 628, an isolated galaxy with ∼ 1/4 the stellar mass of the Milky Way. We present two new dwarf satellite galaxy candidates: NGC 628 dwA, and dwB with MV = −12:2 and −7:7, respectively. NGC 628 dwA is a classical dwarf while NGC 628 dwB is a low-luminosity galaxy that appears to have been quenched after reionization. Com- pleteness corrections indicate that the presence of these two satellites is consistent with CDM predictions. The satellite colors indicate that the galaxies are neither actively star-forming nor do they have the purely ancient stellar populations characteristic of ultrafaint dwarfs. Instead, and consistent with our previous work on the NGC 4214 system, they show signs of recent quenching, further indicating that environmental quenching can play a role in modifying satellite populations even for hosts smaller than the Milky Way. Key words: dwarf { galaxies { local volume 1 INTRODUCTION of large galaxies are well-described by models which use a arXiv:2003.08352v2 [astro-ph.GA] 16 Sep 2020 simple abundance matching prescription to assign galaxies The Λ cold dark matter (CDM) cosmological model pre- to halos after ranking both by mass (Tasitsiomi et al. 2004; dicts the existence of a hierarchy of dark matter halos, in Conroy et al. 2006; Behroozi et al. 2013; Moster et al. 2013). the centers of which galaxies form and reside (see Wechsler However, in the dwarf galaxy regime below this mass scale & Tinker 2018 for a review). This model has had many suc- (M 1010M ), the number, masses and densities of galaxies cesses on large scales. For example, dark-matter-only CDM . predicted by the ΛCDM model are not in clear agreement N-body simulations produce a network of halo structures with observations. This has led researchers to grapple with in remarkable statistical agreement with the spatial distri- the `missing satellites' (e.g., Kauffmann et al. 1993; Moore bution and evolution of massive galaxies (M 1012M ; halo & et al. 1999b; Klypin et al. 1999b), `too big to fail' (Boylan- Schaye et al. 2015; Vogelsberger et al. 2014; Zu & Man- Kolchin et al. 2011) and `cusp-core' (e.g., Flores & Primack delbaum 2015). The global star formation histories (SFH) 1994; Moore 1994; Navarro et al. 1997; Moore et al. 1999a) problems of ΛCDM on small scales (Weinberg et al. 2015; ? E-Mail: [email protected] Bullock & Boylan-Kolchin 2017). © 2020 The Authors 2 A. Bianca Davis et al. One solution to these problems is to modify dark mat- star formation compared to larger galaxies (Tollerud et al. ter particle properties in a way that would change the num- 2011; Simpson et al. 2015; Emerick et al. 2016). In addition, ber of small halos, their expected masses, and densities (Hu internal feedback mechanisms may also modify the density et al. 2000; Vogelsberger et al. 2016; Hui et al. 2017; Lovell profiles of the dark matter halos (Pontzen & Governato 2012; et al. 2017). On the other hand, other probes of small-scale Brooks & Zolotov 2014; Read et al. 2019), changing the map- structure which do not rely on detecting luminous baryons ping between galaxy kinematics and the inferred halo mass, in halos generally show good consistency with CDM. Strong and further altering the M? − Mhalo relation. lensing and Lyman-α forest measurements, as well as mea- There are also indications that environmental effects surements of galaxy abundances in the local Universe, show play an important role in shaping the luminosity function halo mass functions match CDM predictions at mass scales and lives of classical dwarf galaxies, and that these effects de- 7−8 of 10 M (e.g., Weinberg et al. 1997; Dalal & Kochanek pend on satellite galaxy properties. Environmental quench- 2002; Strigari et al. 2007; Tollerud et al. 2008; Behroozi et al. ing mechanisms such as strangulation (Larson et al. 1980), 2010; Reddick et al. 2013; Viel et al. 2013; Baur et al. 2016; ram-pressure (Gunn & Gott 1972) and tidal stripping can Jethwa et al. 2018; Irˇsiˇcet al. 2017; Kim et al. 2018; Nadler also affect dwarf galaxy star formation and quenching times et al. 2019b; Gilman et al. 2020; Nierenberg et al. 2020). as a function of host and satellite mass and orbit (Mayer While there is still a window open for some dark-matter so- et al. 2006; Nichols & Bland-Hawthorn 2011; Wetzel et al. lutions to small-scale structure problems (especially in the 2016; Digby et al. 2019). With the exception of the Large context of halo structure rather than abundance), non-DM and Small Magellanic clouds, all Milky Way satellites are physics is a more likely solution. quenched, while field dwarfs are star-forming (Geha et al. Most of the problems for low mass halos seem to arise 2012), suggesting that environment plays a crucial evolu- because the physics of galaxy formation is not yet sufficiently tionary role for satellites of Milky Way-mass hosts (see also well understood in the context of small dark-matter halos. Slater & Bell 2014; Wetzel et al. 2015; Fillingham et al. Our uncertainties can be cast in terms of the mapping be- 2016). This behavior has been observed in other Mikly Way- tween galaxy stellar and halo masses, the M? − Mhalo rela- mass and larger systems such as M31 (McConnachie & Ir- tion, which is not well-constrained by data below Mhalo = win 2006), M81 (Chiboucas et al. 2013), CenA (Crnoje- 10 10 M . In simulations there is significant variance in the vi´cet al. 2019), and M101 (Bennet et al. 2019). The hot mean relation and in the scatter for halo masses below accretion-shocked gas halos around Milky Way-mass hosts 10 Mhalo = 10 M (Munshi et al. 2013, 2019; Brooks & Zolo- were thought to be necessary to quench satellites through tov 2014; Sawala et al. 2015; Simpson et al. 2015; Fitts et al. strangulation and ram pressure stripping. Lower mass galax- 2017; Wheeler et al. 2019). Predictions of the luminous satel- ies, which are believed to not have hot coronae (Correa et al. lite populations of galaxies are subject to a high degree of 2018), have recently been been shown to have quenched uncertainty even for a well-understood subhalo mass func- satellites (Garling et al. 2020), indicating that intermedi- tion. ate and low mass hosts can also quench star formation in Various global, internal, and environmentally- satellites. dependent astrophysical processes may disproportionately Simple semi-empirical models for the M?−Mhalo relation influence the formation of stars in dwarf galaxies compared coupled with reionization suppression and standard CDM to their more massive counterparts over cosmic time, halo mass functions show good agreement with the Milky complicating the mapping between the luminous dwarf Way's satellite population (Koposov et al. 2008; Tollerud galaxies and their halos. Understanding these processes is et al. 2008; Walsh et al. 2009; Hargis et al. 2014; Jethwa important both for understanding the physics of galaxy et al. 2018; Kim et al. 2018; Newton et al. 2018; Nadler formation, and determining how much room is left for novel et al. 2019a). This appears to solve the `missing satellites dark-matter physics on dwarf galaxy scales. problem' (Klypin et al. 1999a; Moore et al. 1999b), although Globally, reionization could quench star formation on there may still be a deficit of large stellar mass classical small scales, leaving halos below some mass threshold dark dwarfs compared to theoretical predictions (Brooks et al. and completely devoid of luminous baryons (Barkana & 2013; Dooley et al. 2017b; Kim et al. 2018). However, these Loeb 1999; Gnedin 2000; Bullock et al. 2000; Benson et al. models do not incorporate environmental effects, and there 2002; Read & Gilmore 2005; Rodriguez Wimberly et al. is some concern that these semi-empirical models are \over- 2019). We see evidence of this in a new class of `Ultrafaint' tuned" to the Milky Way (Geha et al. 2017; Kim et al. 2018). 5 dwarfs (UFDs) with M? . 10 M , which have been discov- Therefore, to disentangle the various baryonic pro- ered in the Local Group (e.g., Zucker et al. 2004; Willman cesses, and to make better models of, the M?−Mhalo relation et al. 2005; Belokurov et al. 2007; Laevens et al. 2015; Kim as a function of environment, it is necessary to obtain good et al.