Neutral Hydrogen Observations of Low Surface Brightness Galaxies around M101 and NGC 5485

Karunakaran, Ananthan; Spekkens, Kristine; Bennet, Paul; Sand, David J.; Crnojević, Denija; Zaritsky, Dennis

doi:10.3847/1538-3881/ab5af1

Cited by 19 publications

(24 citation statements)

References 65 publications

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“…Converting this to an H i mass limit gives us a 3-σ H i gas mass upper limit of log(M HI /M ) 6.5 (see Table 1). This limit is consistent with the dwarfs being gaspoor, similar to other faint Local Volume dwarf satellites which reside within the virial radius of their primary galaxy (e.g., Grcevich & Putman 2009;Spekkens et al 2014;Karunakaran et al 2020). However, given their low stellar masses, their gas content would not be detectable even if it was relatively high.…”

Section: H I Gas Limitssupporting

confidence: 78%

“…see the recent simulations and discussion in Mutlu-Pakdil et al 2021). Indeed, the census of faint dwarfs around nearby galaxies is well underway using resolved and unresolved imaging (e.g., Chiboucas et al 2013;Sand et al 2014Sand et al , 2015Crnojević et al 2014Crnojević et al , 2016bCrnojević et al , 2019Carlin et al 2016Carlin et al , 2021aToloba et al 2016c;Danieli et al 2017;Smercina et al 2018;Bennet et al 2017Bennet et al , 2019Bennet et al , 2020Carlsten et al 2020;Davis et al 2021;Drlica-Wagner et al 2021;Carlsten et al 2021;Garling et al 2021), as well as spectroscopic surveys around MW analogs at larger distances (Geha et al 2017;Mao et al 2020). These data are already yielding new challenges, with simulations of MW-like galaxies showing a higher fraction and number of quiescent satellites with respect to the observations (Karunakaran et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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Hubble Space Telescope Observations of NGC 253 Dwarf Satellites: Discovery of Three Ultra-faint Dwarf Galaxies

Mutlu-Pakdil,

Sand,

Crnojević

et al. 2021

Preprint

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We present deep Hubble Space Telescope imaging of five faint dwarf galaxies associated with the nearby spiral NGC 253 (D≈3.5 Mpc). Three of these are newly discovered ultra-faint dwarf galaxies, while all five were found in the Panoramic Imaging Survey of Centaurus and Sculptor (PISCeS), a Magellan+Megacam survey to identify faint dwarfs and other substructures in resolved stellar light around massive galaxies outside of the Local Group. Our HST data reach 3 magnitudes below the tip of the red giant branch for each dwarf, allowing us to derive their distances, structural parameters, and luminosities. All five systems contain predominantly old, metal-poor stellar populations (age∼12 Gyr, [M/H] −1.5) and have sizes (r h ∼110-3000 pc) and luminosities (M V ∼−7 to −12 mag) largely consistent with Local Group dwarfs. The three new NGC 253 satellites are among the faintest systems discovered beyond the Local Group. We also use archival H i data to place limits on the gas content of our discoveries. Deep imaging surveys such as our program around NGC 253 promise to elucidate the faint end of the satellite luminosity function and its scatter across a range of galaxy masses, morphologies, and environments in the decade to come.

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Section: H I Gas Limitssupporting

confidence: 78%

Section: Introductionmentioning

confidence: 99%

Hubble Space Telescope Observations of NGC 253 Dwarf Satellites: Discovery of Three Ultra-faint Dwarf Galaxies

Mutlu-Pakdil,

Sand,

Crnojević

et al. 2021

Preprint

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“…With tidal indices of 0.5 and -0.1 respectively we consider M101 and M94 to be relatively isolated compared to other Local Volume hosts such as M31 (Θ 5 =1.8) or M81 (Θ 5 =2.6) ). Follow-up HI observations of a large sample of M101 dwarf candidates confirmed that several were associated with the background galaxy group NGC 5485 via velocity measurements, and that the faintest M101 satellites within the virial radius of M101 are quenched just as those in the Local Group (Karunakaran et al 2020).…”

Section: Introductionmentioning

confidence: 91%

“…Five other diffuse dwarf candidates with M V −8.2 mag from the original CFHTLS sample remain -Dw24, Dw25, Dw29, Dw36 and Dw37 -but their formal distance limits do not overlap with M101 (although Dw24 does overlap at the ∼2-σ level). We note that none of these five dwarfs were targeted in the HI study of Karunakaran et al (2020), but future observations would be beneficial. For the purposes of this work we assume that the SBF distance limits are correct and that these five dwarfs are not viable M101 members.…”

Section: The M101 Satellite Luminosity Functionmentioning

confidence: 99%

The Satellite Luminosity Function of M101 into the Ultra-faint Dwarf Galaxy Regime

Bennet

Sand

Crnojević

et al. 2020

ApJL

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We have obtained deep Hubble Space Telescope (HST) imaging of four faint and ultra-faint dwarf galaxy candidates in the vicinity of M101 -Dw21, Dw22, Dw23 and Dw35, originally discovered by Bennet et al. (2017). Previous distance estimates using the surface brightness fluctuation technique have suggested that these four dwarf candidates are the only remaining viable M101 satellites identified in ground based imaging out to the virial radius of M101 (D≈250 kpc). Advanced Camera for Surveys imaging of all four dwarf candidates shows no associated resolved stellar populations, indicating that they are thus background galaxies. We confirm this by generating simulated HST color magnitude diagrams of similar brightness dwarfs at the distance of M101. Our targets would have displayed clear, resolved red giant branches with dozens of stars if they had been associated with M101. With this information, we construct a satellite luminosity function for M101, which is 90% complete to M V =−7.7 mag and 50% complete to M V =−7.4 mag, that extends into the ultra-faint dwarf galaxy regime. The M101 system is remarkably poor in satellites in comparison to the Milky Way and M31, with only eight satellites down to an absolute magnitude of M V =−7.7 mag, compared to the 14 and 26 seen in the Milky Way and M31, respectively. Further observations of Milky Way analogs are needed to understand the halo-to-halo scatter in their faint satellite systems, and connect them with expectations from cosmological simulations.

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“…The presence of Hα emission or a large reservoir of neutral gas would be a more robust indicator of star formation activity (e.g. Grcevich & Putman 2009;Geha et al 2017;Mao et al 2020;Karunakaran et al 2020). However, since our survey is primarily photometricbased at this point, many of the dwarfs do not have spectra or measurements of their neutral gas.…”

Section: Galaxy Morphologymentioning

confidence: 99%

Structures of Dwarf Satellites of Milky Way-like Galaxies: Morphology, Scaling Relations, and Intrinsic Shapes

Carlsten

Greene

Greco

et al. 2021

ApJ

101

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The structure of a dwarf galaxy is an important probe of the effects of stellar feedback and environment. Using an unprecedented sample of 223 low-mass satellites from the ongoing Exploration of Local Volume Satellites survey, we explore the structures of dwarf satellites in the mass range 105.5 < M ⋆ < 108.5 M ⊙. We survey satellites around 80% of the massive, M K < − 22.4 mag, hosts in the Local Volume (LV). Our sample of dwarf satellites is complete to luminosities of M V <−9 mag and surface brightness μ 0,V < 26.5 mag arcsec−2 within at least ∼200 projected kpc of the hosts. For this sample, we find a median satellite luminosity of M V = −12.4 mag, median size of r e = 560 pc, median ellipticity of ϵ = 0.30, and median Sérsic index of n = 0.72. We separate the satellites into late- and early-type (29.6% and 70.4%, respectively). The mass–size relations are very similar between them within ∼5%, which indicates that the quenching and transformation of a late-type dwarf into an early-type one involves only very mild size evolution. Considering the distribution of apparent ellipticities, we infer the intrinsic shapes of the early- and late-type samples. Combining with literature samples, we find that both types of dwarfs are described roughly as oblate spheroids that get more spherical at fainter luminosities, but early-types are always rounder at fixed luminosity. Finally, we compare the LV satellites with dwarf samples from the cores of the Virgo and Fornax clusters. We find that the cluster satellites show similar scaling relations to the LV early-type dwarfs but are roughly 10% larger at fixed mass, which we interpret as being due to tidal heating in the cluster environments. The dwarf structure results presented here are a useful reference for simulations of dwarf galaxy formation and the transformation of dwarf irregulars into spheroidals.

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Neutral Hydrogen Observations of Low Surface Brightness Galaxies around M101 and NGC 5485

Cited by 19 publications

References 65 publications

Hubble Space Telescope Observations of NGC 253 Dwarf Satellites: Discovery of Three Ultra-faint Dwarf Galaxies

Hubble Space Telescope Observations of NGC 253 Dwarf Satellites: Discovery of Three Ultra-faint Dwarf Galaxies

The Satellite Luminosity Function of M101 into the Ultra-faint Dwarf Galaxy Regime

Structures of Dwarf Satellites of Milky Way-like Galaxies: Morphology, Scaling Relations, and Intrinsic Shapes

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