The feeble giant. Discovery of a large and diffuse Milky Way dwarf galaxy in the constellation of Crater

Torrealba, G.; Koposov, S. E.; Belokurov, V.; Irwin, M. J.

doi:10.1093/mnras/stw733

Cited by 230 publications

(242 citation statements)

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“…Laevens et al 2014Laevens et al , 2015. Milky Way dwarf galaxies are shown as circled dots (data from Irwin & Hatzidimitriou 1995;Martin et al 2008;Belokurov et al 2009Belokurov et al , 2010Laevens et al 2015;Torrealba et al 2016). DECam-enabled discoveries are shown as large dots Drlica-Wagner et al 2015;Kim & Jerjen 2015;Kim et al 2015aKim et al , 2015bKoposov et al 2015, for the Drlica-Wagner et al reference, only high-confidence candidates are considered), except for the two SMASH discoveries that are shown as stars (SMASH 1, which appears in yellow at the bottom of the plot, and Hya II; Martin et al 2015).…”

Section: Discussionmentioning

confidence: 99%

Smash 1: A Very Faint Globular Cluster Disrupting in the Outer Reaches of the Lmc?

Martín

Jungbluth

Nidever

et al. 2016

ApJL

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We present the discovery of a very faint stellar system, SMASH 1, that is potentially a satellite of the Large Magellanic Cloud. Found within the Survey of the MAgellanic Stellar History (SMASH), SMASH 1 is a compact ( r 9.1 pc h 3.4 5.9) and very low luminosity ( M) stellar system that is revealed by its sparsely populated main sequence and a handful of red giant branch candidate member stars. The photometric properties of these stars are compatible with a metal-poor ( Fe H 2.2 [ ] ) and old (13 Gyr) isochrone located at a distance modulus of ∼18.8, i.e., a distance of 57 kpc. Situated at 11°. 3 from the LMC in projection, its three-dimensional distance from the Cloud is 13 kpc, consistent with a connection to the LMC, whose tidal radius is at least 16 kpc. Although the nature of SMASH 1 remains uncertain, its compactness favors it being a stellar cluster and hence dark-matter free. If this is the case, its dynamical tidal radius is only 19 pc at this distance from the LMC, and smaller than the system's extent on the sky. Its low luminosity and apparent high ellipticity ( 0.62 0.21 0.17 ) with its major axis pointing toward the LMC may well be the tell-tale sign of its imminent tidal demise.

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Section: Discussionmentioning

confidence: 99%

Smash 1: A Very Faint Globular Cluster Disrupting in the Outer Reaches of the Lmc?

Martín

Jungbluth

Nidever

et al. 2016

ApJL

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“…Over the past two years, more than 20 ultra-faint dwarf galaxy candidates have been discovered in data from the Dark Energy Survey (DES; Bechtol et al 2015;Drlica-Wagner et al 2015b;Kim & Jerjen 2015;Koposov et al 2015) and other large optical surveys (Kim et al 2015a(Kim et al , 2015bLaevens et al 2015bLaevens et al , 2015aMartin et al 2015;Drlica-Wagner et al 2016;Homma et al 2016;Torrealba et al 2016aTorrealba et al , 2016b. One of the largest most luminous and most distant newly discovered satellites is EridanusII (Eri II), which has an absolute magnitude of M V ∼−7, a half-light radius of r h ∼280 pc, and a Galactocentric distance of D∼370 kpc (Bechtol et al 2015;Koposov et al 2015;Crnojević et al 2016; see Table 1).…”

Section: Introductionmentioning

confidence: 99%

Farthest Neighbor: The Distant Milky Way Satellite Eridanus II*

Simon

Drlica-Wagner

et al. 2017

ApJ

151

153

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We present Magellan/IMACS spectroscopy of the recently discovered Milky Way satellite EridanusII (Eri II).We identify 28 member stars in EriII, from which we measure a systemic radial velocity of () 1 the bright blue stars previously suggested to be a young stellar population are not associated with EriII. The lack of gas and recent star formation in EriII is surprising given its mass and distance from the Milky Way, and may place constraints on models of quenching in dwarf galaxies and on the distribution of hot gas in the Milky Way halo. Furthermore, the large velocity dispersion of Eri II can be combined with the existence of a central star cluster to constrain massive compact halo object dark matter with mass 10  M .

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“…The discovery of Milky Way satellites in the last few years has reached an extremely rapid pace, with the total number of objects found since 2015 nearly matching the entire previously known population (Bechtol et al 2015;Drlica-Wagner et al 2015bKim & Jerjen 2015;Kim et al 2015aKim et al , 2015bKoposov et al 2015a;Laevens et al 2015aLaevens et al , 2015bMartin et al 2015;Torrealba et al 2016aTorrealba et al , 2016b. The photometric identification of these objects in the Dark Energy Survey (DES) and other large surveys has far outstripped the spectroscopic follow-up efforts needed to characterize them.…”

Section: Introductionmentioning

confidence: 99%

Nearest Neighbor: The Low-mass Milky Way Satellite Tucana III*

Simon¹,

Li²,

Drlica-Wagner³

et al. 2017

ApJ

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We present Magellan/IMACS spectroscopy of the recently discovered Milky Way satellite Tucana III (Tuc III). We identify 26 member stars in Tuc III, from which we measure a mean radial velocity of v hel = −102.3 ± 0.4 (stat.) ± 2.0 (sys.) km s −1 , a velocity dispersion of 0.1 +0.7 −0.1 km s −1 , and a mean metallicity of [Fe/H] = −2.42 +0.07 −0.08 . The upper limit on the velocity dispersion is σ < 1.5 km s −1 at 95.5% confidence, and the corresponding upper limit on the mass within the half-light radius of Tuc III is 9.0 × 10 4 M . We cannot rule out mass-to-light ratios as large as 240 M / L for Tuc III, but much lower mass-to-light ratios that would leave the system baryon-dominated are also allowed. We measure an upper limit on the metallicity spread of the stars in Tuc III of 0.19 dex at 95.5% confidence. Tuc III has a smaller metallicity dispersion and likely a smaller velocity dispersion than any known dwarf galaxy, but a larger size and lower surface brightness than any known globular cluster. Its metallicity is also much lower than those of the clusters with similar luminosity. We therefore tentatively suggest that Tuc III is the tidally-stripped remnant of a dark matter-dominated dwarf galaxy, but additional precise velocity and metallicity measurements will be necessary for a

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The feeble giant. Discovery of a large and diffuse Milky Way dwarf galaxy in the constellation of Crater

Cited by 230 publications

References 50 publications

Smash 1: A Very Faint Globular Cluster Disrupting in the Outer Reaches of the Lmc?

Smash 1: A Very Faint Globular Cluster Disrupting in the Outer Reaches of the Lmc?

Farthest Neighbor: The Distant Milky Way Satellite Eridanus II*

Nearest Neighbor: The Low-mass Milky Way Satellite Tucana III*

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