DGSAT: Dwarf Galaxy Survey with Amateur Telescopes

Henkel, C.; Javanmardi, Behnam; Martínez–Delgado, David; Kroupa, Pavel; Teuwen, R.

doi:10.1051/0004-6361/201730539

Cited by 26 publications

(24 citation statements)

References 57 publications

(66 reference statements)

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“…The 3σ standard deviation -transformed to the r-band using the linear photomet-ric transformation -is µ lim,r = 28.5 mag arcsec −2 . This limit is comparable to the depth reached by other telescopes of modest aperture size (Martínez-Delgado et al 2010;Karachentsev et al 2015;Javanmardi et al 2016;Henkel et al 2017).…”

Section: Observations and Data Processingsupporting

confidence: 54%

A tidal tale: detection of several stellar streams in the environment of NGC 1052

Müller

Rich

Román

et al. 2019

A&A

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The possible existence of two dark matter free galaxies (NGC1052-DF2 and NGC1052-DF4) in the field of the early-type galaxy NGC 1052 presents a challenge to theories of dwarf galaxy formation according to the current cosmological paradigm. We carried out a search for signatures of past interactions connected to the putative hosts of NGC 1052-DF2 and NGC 1052-DF4 using a very deep L-band image obtained with the 0.7 m Jeanne Rich telescope that reach a surface brightness limit of 28.5 mag arcsec −2 in the r band. We found several low-surface brightness features, possibly consistent with an ongoing merger history in this group. We find a tidal interaction between NGC 1052 and NGC 1047, confirming a physical association. Furthermore we find a stellar loop around NGC 1052 in the direction of NGC 1042 and a stellar stream pointing in the direction of NGC 1052-DF2 -but both are not directly connected. We find no evidence for a recent tidal interaction for NGC 1052-DF2 and NGC 1052-DF4. No low surface brightness features have been uncovered around the spiral galaxy NGC 1042, which leaves the association (physical or projected) between NGC 1052 and NGC 1042 ambiguous, though they have similar radial velocities. Their association will only be established once accurate distances to both objects have been measured.

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Section: Observations and Data Processingsupporting

confidence: 54%

A tidal tale: detection of several stellar streams in the environment of NGC 1052

Müller

Rich

Román

et al. 2019

A&A

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“…These galaxies must obviously have a wide range of M bulge . In fact, for the DGSAT project, Henkel et al (2017) have already compiled a catalog of more than 30 edge-on disk galaxies with similar luminosities and with distances 40 Mpc for the exact same purpose.…”

Section: Discussionmentioning

confidence: 99%

The Number of Dwarf Satellites of Disk Galaxies versus their Bulge Mass in the Standard Model of Cosmology

Raouf

Khosroshahi

Tavasoli

et al. 2019

ApJ

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There is a correlation between bulge mass of the three main galaxies of the Local Group (LG), i.e. M31, Milky Way (MW), and M33, and the number of their dwarf spheroidal galaxies. A similar correlation has also been reported for spiral galaxies with comparable luminosities outside the LG. These correlations do not appear to be expected in standard hierarchical galaxy formation. In this contribution, and for the first time, we present a quantitative investigation of the expectations of the standard model of cosmology for this possible relation using a galaxy catalogue based on the Millennium-II simulation. Our main sample consists of disk galaxies at the centers of halos with a range of virial masses similar to M33, MW, and M31. For this sample, we find an average trend (though with very large scatter) similar to the one observed in the LG; disk galaxies in heavier halos on average host heavier bulges and larger number of satellites. In addition, we study sub-samples of disk galaxies with very similar stellar or halo masses (but spanning a range of 2-3 orders of magnitude in bulge mass) and find no obvious trend in the number of satellites vs. bulge mass. We conclude that while for a wide galaxy mass range a relation arises (which seems to be a manifestation of the satellite number -halo mass correlation), for a narrow one there is no relation between number of satellites and bulge mass in the standard model. Further studies are needed to better understand the expectations of the standard model for this possible relation.

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“…With sizes of 70 r eff pc 300, these objects are broadly consistent with properties of LG dSphs, in particular those that show the highest stellar surface densities, and have many analogues in the Local Volume (LV; Chiboucas et al 2009;McConnachie 2012;Müller et al 2015Müller et al , 2017a, see also Fig.3). Figure 3 compares the modeled r eff and total luminosities to other low-mass stellar systems in the NGC 5128-M83 complex (Crnojević et al 2014(Crnojević et al , 2016Müller et al 2015Müller et al , 2017a, and for additional context to various other dwarfs in the LV, including the M81, M101, M96, and Leo systems (Chiboucas et al 2009;Merritt et al 2014;Javanmardi et al 2016;Bennet et al 2017;Henkel et al 2017;Park et al 2017;Müller et al 2017bMüller et al , 2018a, and the Fornax galaxy cluster core (Muñoz et al 2015;Eigenthaler et al 2018). We also show low-mass satellites identified in the LG (McConnachie 2012; Bechtol et al 2015;Smercina et al 2017;Homma et al 2018;Muñoz et al 2018b).…”

Section: Analysis 31 Dwarf Detection and Photometric Analysismentioning

confidence: 99%

A Collection of New Dwarf Galaxies in NGC 5128’s Western Halo

Taylor

Eigenthaler

Puzia

et al. 2018

ApJL

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We report the photometric properties of 16 dwarf galaxies, 15 of which are newly identified, in the Western halo of the nearby giant elliptical galaxy NGC 5128. All candidates are found at projected distances ∼ 100 − 225 kpc from their giant host, with luminosities −10.82 ≤ M V mag ≤ −7.42 and effective radii 4 ′′ r eff 17 ′′ (or 75 r eff pc 300 at the distance of NGC 5128). We compare to other low-mass dwarf galaxies in the local universe and find them to populate the faint/compact extension of the size-luminosity relation that was previously not well-sampled by dwarf galaxies in the Centaurus A system, with optical colors similar to compact stellar systems like globular clusters and ultra-compact dwarf galaxies despite having much more diffuse morphologies. From optical u ′ g ′ r ′ i ′ z ′ photometry, stellar masses are estimated to be 5.17≤logM ⋆ M ⊙ ≤ 6.48, with colors that show them to fall redward of the dwarf galaxy mass-metallicity relation. These colors suggest star formation histories that require some mechanism that would give rise to extra metal enrichment such as primordial formation within the halos of their giant galaxy hosts, non-primordial star formation from previously enriched gas, or extended periods of star formation leading to self-enrichment. We also report the existence of at least two sub-groups of dwarf candidates, each subtending 15 ′ on the sky, corresponding to projected physical separations of 10−20 kpc. True physical associations of these groups, combined with their potentially extended star formation histories, would imply that they may represent dwarf galaxy groups in the early stage of interaction upon infall into a giant elliptical galaxy halo in the very nearby universe.

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DGSAT: Dwarf Galaxy Survey with Amateur Telescopes

Cited by 26 publications

References 57 publications

A tidal tale: detection of several stellar streams in the environment of NGC 1052

A tidal tale: detection of several stellar streams in the environment of NGC 1052

The Number of Dwarf Satellites of Disk Galaxies versus their Bulge Mass in the Standard Model of Cosmology

A Collection of New Dwarf Galaxies in NGC 5128’s Western Halo

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