Direct evidence of hierarchical assembly at low masses from isolated dwarf galaxy groups

Stierwalt, Sabrina; Liss, S.; Johnson, K. E.; Patton, David R.; Privon, George C.; Besla, Gurtina; Kallivayalil, Nitya; Putman, Mary E.

doi:10.1038/s41550-016-0025

Cited by 42 publications

(45 citation statements)

References 47 publications

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“…We have to contend, though, with the fact that while the coverage is extensive it is not complete. In any event, our results are consistent with the claim by Stierwalt et al (2017) based on the statistics of dwarf correlations at larger distances that bound multiple systems of dwarfs are rare.…”

Section: Special Case: Nearest 10 Mpcsupporting

confidence: 92%

Galaxy Groups Within 3500 km s⁻¹

Kourkchi¹,

Tully²

2017

ApJ

206

232

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A study of the group properties of galaxies in our immediate neighborhood provides a singular opportunity to observationally constrain the halo mass function, a fundamental characterization of galaxy formation. Detailed studies of individual groups have provided the coefficients of scaling relations between a proxy for the virial radius, velocity dispersion, and mass that usefully allows groups to be defined over the range 10 10 −10 15 M ⊙ . At a second hierarchical level, associations are defined as regions around collapsed halos extending to the zero velocity surface at the decoupling from cosmic expansion. The most remarkable result of the study emerges from the construction of the halo mass function from the sample. At ∼ 10 12 M ⊙ there is a jog from the expectation Sheth-Tormen function, such that halo counts drop by a factor ∼ 3 in all lower mass bins.

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Section: Special Case: Nearest 10 Mpcsupporting

confidence: 92%

Galaxy Groups Within 3500 km s⁻¹

Kourkchi¹,

Tully²

2017

ApJ

206

232

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“…D'Onghia & Lake 2008) and observations (e.g. Tully et al 2006;Stierwalt et al 2017), and in this case would point to a MW analog accreting a group of dwarfs. This idea is reinforced by the highly asymmetric HI and optical disk of M101 (Mihos et al 2012, Mihos et al 2013, which show features extending away from the disk to the east and northeast.…”

Section: Distribution Of New Dwarfs Around M101mentioning

confidence: 99%

Discovery of Diffuse Dwarf Galaxy Candidates around M101

Bennet

Sand

Crnojević

et al. 2017

ApJ

106

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We have conducted a search of a 9 deg 2 region of the CFHTLS around the Milky Way analog M101 (D∼7 Mpc), in order to look for previously unknown low surface brightness galaxies. This search has uncovered 38 new low surface brightness dwarf candidates, and confirmed 11 previously reported galaxies, all with central surface brightness µ(g,0)>23mag/arcsec 2 , potentially extending the satellite luminosity function for the M101 group by ∼1.2 magnitudes. The search was conducted using an algorithm that nearly automates the detection of diffuse dwarf galaxies. The candidates small size and low surface brightness means that the faintest of these objects would likely be missed by traditional visual or computer detection techniques. The dwarf galaxy candidates span a range of −7.1 ≥ M g ≥ −10.2 and half light radii of 118-540 pc at the distance of M101, and they are well fit by simple Sérsic surface brightness profiles. These properties are consistent with dwarfs in the Local Group, and to match the Local Group luminosity function ∼10-20 of these candidates should be satellites of M101. Association with a massive host is supported by the lack of detected star formation and the over density of candidates around M101 compared to the field. The spatial distribution of the dwarf candidates is highly asymmetric, and concentrated to the northeast of M101 and therefore distance measurements will be required to determine if these are genuine members of the M101 group.

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“…satellites of the Milky Way (Newton et al 2018;Muñoz et al 2018) or Local Group members (Drlica-Wagner et al 2015), with the MADCASH survey being an exception (Carlin et al 2016). Another recent important result is the discovery of seven galaxy groups composed purely of dwarf galaxies (Stierwalt et al 2017), confirming theoretical predictions that primordial density fluctuations should be scale-free and that in some cases, dwarf galaxy populations can evolve in a similar way to their more massive counterparts.…”

Section: Introductionmentioning

confidence: 66%

Evolution of dwarf galaxy observable parameters

Ledinauskas

Zubovas

2020

Monthly Notices of the Royal Astronomical Society

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We present a semi-analytic model of isolated dwarf galaxy evolution and use it to study the build-up of observed correlations between dwarf galaxy properties. We analyse the evolution using models with averaged and individual halo mass assembly histories in order to determine the importance of stochasticity on the present-day properties of dwarf galaxies. The model has a few free parameters, but when these are calibrated using the halo mass -stellar mass and stellar mass-metallicity relations, the results agree with other observed dwarf galaxy properties remarkably well. Redshift evolution shows that even isolated galaxies change significantly over the Hubble time and that 'fossil dwarf galaxies' with properties equivalent to those of high-redshift analogues should be extremely rare, or non-existent, in the local Universe. A break in most galaxy property correlations develops over time, at a stellar mass M * 10 7 M . It is caused predominantly by the ionizing background radiation and can therefore in principle be used to constrain the properties of reionization.

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Direct evidence of hierarchical assembly at low masses from isolated dwarf galaxy groups

Cited by 42 publications

References 47 publications

Galaxy Groups Within 3500 km s⁻¹

Galaxy Groups Within 3500 km s⁻¹

Discovery of Diffuse Dwarf Galaxy Candidates around M101

Evolution of dwarf galaxy observable parameters

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Direct evidence of hierarchical assembly at low masses from isolated dwarf galaxy groups

Cited by 42 publications

References 47 publications

Galaxy Groups Within 3500 km s−1

Galaxy Groups Within 3500 km s−1

Discovery of Diffuse Dwarf Galaxy Candidates around M101

Evolution of dwarf galaxy observable parameters

Contact Info

Product

Resources

About

Galaxy Groups Within 3500 km s⁻¹

Galaxy Groups Within 3500 km s⁻¹