The Exploration of Local VolumE Satellites (ELVES) Survey: A Nearly Volume-limited Sample of Nearby Dwarf Satellite Systems

Carlsten, Scott G.; Greene, Jenny E.; Beaton, Rachael L.; Danieli, Shany; Greco, Johnny P.

doi:10.3847/1538-4357/ac6fd7

Cited by 69 publications

(160 citation statements)

References 249 publications

Supporting

Mentioning

125

Contrasting

Order By: Relevance

“…Their close proximities have enabled discovery and detailed characterization over a large dynamic range in stellar mass that is not possible to match in other environments (e.g., Willman et al 2005;Kallivayalil et al 2006Kallivayalil et al , 2013Belokurov et al 2007;Besla et al 2007;Simon & Geha 2007;Kirby et al 2008;van der Marel & Kallivayalil 2014;Bechtol et al 2015;Koposov et al 2015;Fritz et al 2018;Simon 2019). While substantial efforts are being made to identify and study low-mass satellites throughout the Local Volume in order to test the representative nature of the MW satellite population (e.g., Chiboucas et al 2009;Dalcanton et al 2009;Calzetti et al 2015;Geha et al 2017;Smercina et al 2018;Bennet et al 2019;Crnojević et al 2019;Okamoto et al 2019;Carlsten et al 2020Carlsten et al , 2022Drlica-Wagner et al 2021;Mao et al 2021), they are generally limited to fairly bright systems and coarse characterizations of their stellar populations (e.g., Da Costa et al 2010;Weisz et al 2011;Cignoni et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure

Savino

Weisz

Skillman

et al. 2022

ApJ

View full text Add to dashboard Cite

We measure homogeneous distances to M31 and 38 associated stellar systems (−16.8 ≤ M V ≤ −6.0), using time-series observations of RR Lyrae stars taken as part of the Hubble Space Telescope Treasury Survey of M31 Satellites. From >700 orbits of new/archival Advanced Camera for Surveys imaging, we identify >4700 RR Lyrae stars and determine their periods and mean magnitudes to a typical precision of 0.01 day and 0.04 mag. Based on period–Wesenheit–metallicity relationships consistent with the Gaia eDR3 distance scale, we uniformly measure heliocentric and M31-centric distances to a typical precision of ∼20 kpc (3%) and ∼10 kpc (8%), respectively. We revise the 3D structure of the M31 galactic ecosystem and: (i) confirm a highly anisotropic spatial distribution such that ∼80% of M31's satellites reside on the near side of M31; this feature is not easily explained by observational effects; (ii) affirm the thin (rms 7–23 kpc) planar “arc” of satellites that comprises roughly half (15) of the galaxies within 300 kpc from M31; (iii) reassess the physical proximity of notable associations such as the NGC 147/185 pair and M33/AND xxii; and (iv) illustrate challenges in tip-of-the-red-giant branch distances for galaxies with M V > − 9.5, which can be biased by up to 35%. We emphasize the importance of RR Lyrae for accurate distances to faint galaxies that should be discovered by upcoming facilities (e.g., Rubin Observatory). We provide updated luminosities and sizes for our sample. Our distances will serve as the basis for future investigation of the star formation and orbital histories of the entire known M31 satellite system.

show abstract

Section: Introductionmentioning

confidence: 99%

The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure

Savino

Weisz

Skillman

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

“…MNRAS 516, 1741-1751 (2022) These studies, whether via integrated light (Merritt, van Dokkum & Abraham (Merritt, van Dokkum & Abraham 2014 ;Karachentsev et al 2015 ;Javanmardi et al 2016 ;Bennet et al 2017 ;Geha et al 2017 ;M üller et al 2017 ;Smercina et al 2018 ;Carlsten et al 2019Carlsten et al , 2022aMao et al 2021 ) or via resolved stars (Chiboucas, Karachentsev & Tully 2009 ;Chiboucas et al 2013 ;Carlin et al 2016 ;Crnojevi ć et al 2016Crnojevi ć et al , 2019Bennet et al 2019Bennet et al , 2020Mutlu-Pakdil et al 2021, have discovered dozens of new satellites in nearby systems. These growing samples enable increasingly detailed comparisons to the Local Group satellite system.…”

mentioning

confidence: 99%

H i properties of satellite galaxies around local volume hosts

Karunakaran

Spekkens

Carroll

et al. 2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present neutral atomic hydrogen (H i) observations using the Robert C. Byrd Green Bank Telescope (GBT) along the lines of sight to 49 confirmed or possible dwarf satellite galaxies around eight Local Volume systems (M104, M51, NGC 1023, NGC 1156, NGC 2903, NGC 4258, NGC 4565, NGC 4631). We detect the H i reservoirs of two candidates (dw0934+2204 and dw1238−1122) and find them to be background sources relative to their nearest foreground host systems. The remaining 47 satellite candidates are not detected in H i, and we place stringent 5σ upper limits on their H i mass. We note that some (15/47) of our non-detections stem from satellites being occluded by their putative host’s H i emission. In addition to these new observations, we compile literature estimates on the H i mass for an additional 17 satellites. We compare the H i properties of these satellites to those within the Local Group, finding broad agreement between them. Crucially, these observations probe a ‘transition’ region between −10 ≳ MV ≳ −14 where we see a mixture of gas-rich and gas-poor satellites. While there are many gas-poor satellites within this region, some are gas-rich and this suggests that the transition towards predominantly gas-rich satellites occurs at LV ∼ 107L⊙, in line with simulations. The observations presented here are a key step toward characterizing the properties of dwarf satellite galaxies around Local Volume systems and future wide-field radio surveys with higher angular resolution (e.g. WALLABY) will vastly improve upon the study of such systems.

show abstract

“…Measurements of quenched fractions for faint satellite galaxies have also been obtained recently for nearby systems similar to the Local Group. In Figure 12 the old fraction of galaxies as a function of M r obtained by us for Milky Way-like halos with 12.0 ≤ (M h /M ) < 12.34, in comparison with the quenched fractions obtained by Wetzel et al (2015) for the MW+M31 system, by Geha et al (2017) and Mao et al (2021) using the SAGA survey of 127 satellite galaxies around 36 Milky Way (MW) analogs at z ∼ 0.01, and by Carlsten et al (2022) and Karunakaran et al (2022) using the ELVES survey of a nearly volume-limited sample of dwarf satellites down to M V ∼ −9. Our result is in good agreement with the result of both the MW+M31 halo and the ELVES survey.…”

Section: Comparisons With Previous Observationsmentioning

confidence: 88%

Galaxy populations in groups and clusters: evidence for a characteristic stellar mass scale at $M_\ast\sim 10^{9.5}M_\odot$

Meng¹,

Li²,

Mo³

et al. 2022

Preprint

View full text Add to dashboard Cite

We use the most recent data release (DR9) of the DESI legacy imaging survey and SDSS galaxy groups to measure the conditional luminosity function (CLF) for groups with halo mass M h ≥ 10 12 M and redshift 0.01 ≤ z ≤ 0.08, down to a limiting r-band magnitude of M r = −10 ∼ −12. For a given halo mass we measure the CLF for the total satellite population, as well as separately for the red and blue populations classified using the (g − z) color. We find a clear faint-end upturn in the CLF of red satellites, with a slope α ≈ −1.8 which is almost independent of halo mass. This faint-end upturn is not seen for blue satellites and for the total population. Our stellar population synthesis modeling shows that the (g − z) color provides a clean red/blue division, and that group galaxies in the red population defined by (g − z) are all dominated by old stellar populations. The fraction of old galaxies as a function of galaxy luminosity shows a minimum at a luminosity M r ∼ −18, corresponding to a stellar mass M * ∼ 10 9.5 M . This mass scale is independent of halo mass and is comparable to the characteristic luminosity at which galaxies show a dichotomy in surface brightness and size, suggesting that the dichotomy in the old fraction and in galaxy structure may have a common origin. The rising of the old fraction at the faint end for Milky Way (MW)-sized halos found here is in good agreement with the quenched fraction measured both for the MW/M31 system and from the ELVES survey. We discuss the implications of our results for the formation and evolution of low-mass galaxies, and for the stellar mass functions of low-mass galaxies to be observed at high redshift.

show abstract

The Exploration of Local VolumE Satellites (ELVES) Survey: A Nearly Volume-limited Sample of Nearby Dwarf Satellite Systems

Abstract: We present the final sample of the Exploration of Local VolumE Satellites (ELVES) survey, a survey of the dwarf satellites of a nearly volume-limited sample of Milky Way (MW)−like hosts in the Local Volume. Hosts are selected simply via a cut in luminosity ( M … Show more

Cited by 69 publications

References 249 publications

The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure

The Hubble Space Telescope Survey of M31 Satellite Galaxies. I. RR Lyrae–based Distances and Refined 3D Geometric Structure

H i properties of satellite galaxies around local volume hosts

Galaxy populations in groups and clusters: evidence for a characteristic stellar mass scale at $M_\ast\sim 10^{9.5}M_\odot$

Contact Info

Product

Resources

About