Dwarf Spheroidal Galaxies in the M101 Group and Behind it

Караченцев, И. Д.; Макарова, Л. Н.

doi:10.1007/s10511-019-09582-7

Cited by 10 publications

(9 citation statements)

References 20 publications

(28 reference statements)

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“…are shown as yellow circles. For reference, the open square shows the location of M101 in the foreground.The open grey circle centered on NGC 5485 has a radius of 300 kpc at its distance, representative of literature estimates for the virial radius of the corresponding group(Tully 2015;Saulder et al 2016;Karachentsev & Makarova 2019). of similar stellar mass, in line with theoretical expectations.…”

supporting

confidence: 81%

“…The HI detections correspond to galaxies on the group outskirts that have not lost their gas or have yet to be processed by the group environment. NGC 5485 has stellar streamlike features which are likely due to past interactions (Karachentsev & Makarova 2019), further supporting this scenario.…”

Section: Hi Non-detections and The Ngc 5485 Groupmentioning

confidence: 61%

“…This tension is alleviated somewhat by the presence of a background group in the vicinity of M101 (D BG ∼ 27 Mpc, V BG ∼ 1961 km s −1 ; Merritt et al 2016;Tully 2015), which includes the massive ellipticals NGC 5485 and NGC 5473 among its ∼ 25 members (Karachentsev & Makarova 2019;Saulder et al 2016). Indeed, follow-up observations to characterize the properties of the LSB dwarf candidates around M101 suggest that many lie at the distance of the NGC 5485 group (Merritt et al 2016;Bennet et al 2019;Carlsten et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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

Karunakaran

Spekkens

Bennet

et al. 2020

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We present atomic hydrogen (HI) observations using the Robert C. Byrd Green Bank Telescope along the lines-of-sight to 27 low surface brightness (LSB) dwarf galaxy candidates discovered in optical searches around M101. We detect HI reservoirs in 5 targets and place stringent upper limits on the remaining 22, implying that they are gas poor. The distances to our HI detections range from 7 Mpc -150 Mpc, demonstrating the utility of wide-bandpass HI observations as a follow-up tool. The systemic velocities of 3 detections are consistent with that of the NGC 5485 group behind M101, and we suggest that our 15 non-detections with lower distance limits from the optical are associated with and have been stripped by that group. We find that the gas richnesses of confirmed M101 satellites are broadly consistent with those of the Milky Way satellites, as well as with those of satellites around other hosts of comparable mass, when survey completeness is taken into account. This suggests that satellite quenching and gas stripping proceeds similarly around halos of similar mass, in line with theoretical expectations.

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supporting

confidence: 81%

Section: Hi Non-detections and The Ngc 5485 Groupmentioning

confidence: 61%

Section: Introductionmentioning

confidence: 99%

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

Karunakaran

Spekkens

Bennet

et al. 2020

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“…8 (J2000). It is not in the sample of faint low surface brightness objects of Carlsten et al (2019), and given its proximity to M101 it is unlikely that it is a member of the background NGC 5485 group (see Merritt et al 2016b, Karachentsev & Makarova 2019. Its r-band magnitude in the Dragonfly data is m r ≈ 21.2.…”

Section: Masking Of Artifacts In the Final Residual Imagementioning

confidence: 99%

Multi-resolution filtering: an empirical method for isolating faint, extended emission in Dragonfly data and other low resolution images

van Dokkum,

Lokhorst,

Danieli

et al. 2019

Preprint

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We describe an empirical, self-contained method to isolate faint, large-scale emission in imaging data of low spatial resolution. Multi-resolution filtering (MRF) uses independent data of superior spatial resolution to create a model for all compact and high surface brightness objects in the field. This model is convolved with an appropriate kernel and subtracted from the low resolution image. The halos of bright stars are removed in a separate step and artifacts are masked. The resulting image only contains extended emission fainter than a pre-defined surface brightness limit. The method was developed for the Dragonfly Telephoto Array, which produces images that have excellent low surface brightness sensitivity but poor spatial resolution. We demonstrate the MRF technique using Dragonfly images of a satellite of the spiral galaxy M101, the tidal debris surrounding M51, and two ultra-diffuse galaxies in the Coma cluster. As part of the analysis we present a newly-identified very faint galaxy in the filtered Dragonfly image of the M101 field. We also discuss variations of the technique for cases when no low resolution data are available (self-MRF and cross-MRF), and introduce a new method for robustly measuring the surface brightness depth of images. All codes are implemented in mrf, an open-source MIT licensed Python package. a)

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“…Within the Local Group, the satellite dwarfs of the Milky Way (e.g., the MegaCam Survey of Outer Halo Satellites, Marchi-Lasch et al 2019) and those around M31 (e.g., the Pan-Andromeda Archaeological Survey, McConnachie et al 2009;Martin et al 2016) are generally well studied. Typically, these ground-based, resolved stellar studies are limited to the Local Group and work in concert with the extensive number of surveys and studies at larger distances (e.g., M101: Karachentsev & Makarova 2019;Müller et al 2017; Cen A: Müller et al 2019;Crnojević et al 2018;NGC 1291: Byun et al 2020, in other environments (e.g., NGVS Ferrarese et al 2012and Fornax Venhola et al 2018, and which question the "stereotypical" nature of the Local Group (e.g., the SAGA Survey: Geha et al 2017;Mao et al 2020;Carlsten et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Solo dwarfs II: The stellar structure of isolated Local Group dwarf galaxies

Higgs,

McConnachie,

Annau

et al. 2021

Preprint

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The Solo (Solitary Local) Dwarf Galaxy survey is a volume limited, wide-field 𝑔− and 𝑖−band survey of all known nearby (<3 Mpc) and isolated (>300 kpc from the Milky Way or M31) dwarf galaxies. This set of 44 dwarfs are homogeneously analysed for quantitative comparisons to the satellite dwarf populations of the Milky Way and M31. In this paper, an analysis of the 12 closest Solo dwarf galaxies accessible from the northern hemisphere is presented, including derivation of their distances, spatial distributions, morphology, and extended structures, including their inner integrated light properties and their outer resolved star distributions. All 12 galaxies are found to be reasonably well described by two-dimensional Sérsic functions, although UGC 4879 in particular shows tentative evidence of two distinct components. No prominent extended stellar substructures, that could be signs of either faint satellites or recent mergers, are identified in the outer regions of any of the systems examined.

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Dwarf Spheroidal Galaxies in the M101 Group and Behind it

Cited by 10 publications

References 20 publications

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

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

Multi-resolution filtering: an empirical method for isolating faint, extended emission in Dragonfly data and other low resolution images

Solo dwarfs II: The stellar structure of isolated Local Group dwarf galaxies

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