Discovery of a Stellar Overdensity in Eridanus–phoenix in the Dark Energy Survey

Li, T. S.; Balbinot, E.; Mondrik, Nicholas; Marshall, J. L.; Yanny, B.; Bechtol, K.; Drlica-Wagner, A.; Oscar, D.; Santiago, B.; Simon, Joshua D.; Vivas, A. K.; Walker, A. R.; Wang, M. Y.; Abbott, T. M. C.; Abdalla, F. B.; Benoit-Lévy, A.; Bernstein, G. M.; Bertin, E.; Burke, D. L.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Costa, L. N. da; DePoy, D. L.; Desai, S.; Diehl, H. T.; Doel, P.; Estrada, J.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gruen, D.; Gruendl, R. A.; Gutiérrez, G.; Honscheid, K.; James, D. J.; Kuêhn, K.; Kuropatkin, N.; Lahav, O.; Maia, M. A. G.; March, M.; Martini, Paul; Ogando, R. L. C.; Plazas, A. A.; Reil, K.; Romer, A. K.; Sánchez, E.; Scarpine, V.; Schubnell, M.; Sevilla-Noarbe, I.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Suchyta, E.; Swanson, M. E. C.; Tarlè, G.; Tucker, D. L.; Zhang, Y.

doi:10.3847/0004-637x/817/2/135

Cited by 44 publications

(53 citation statements)

References 87 publications

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“…For comparison, the surface brightness of the Virgo Overdensity discovered by SDSS is Σr ∼ 32.5 mag arcsec −2 (Jurić et al 2008), and the surface brightness of the Sagittarius dwarf Northern stream is ΣV ∼ 31 mag arcsec −2 (Martínez- Delgado et al 2004). The stellar overdensity in Eridanus-Phoenix recently discovered by DES has Σr ∼ 32.8 mag arcsec −2 (Li et al 2016). These magnitudes are comparable to the surface brightness of the tidal feature from F2, therefore similar features could be detected in ongoing or existing imaging surveys.…”

Section: Surface Densities Of Stellar Tidal Featuressupporting

confidence: 52%

Tidal features of classical Milky Way satellites in a Λ cold dark matter universe

Wang

Fattahi

Cooper

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use the APOSTLE cosmological hydrodynamic simulations to examine the effects of tidal stripping on cold dark matter (CDM) subhaloes that host three of the most luminous Milky Way (MW) dwarf satellite galaxies: Fornax, Sculptor, and Leo I. We identify simulated satellites that match the observed spatial and kinematic distributions of stars in these galaxies, and track their evolution after infall. We find ∼ 30% of subhaloes hosting satellites with present-day stellar mass 10 6 -10 8 M ⊙ experience > 20% stellar mass loss after infall. Fornax analogues have earlier infall times compared to Sculptor and Leo I analogues. Star formation in Fornax analogues continues for ∼ 3-6 Gyr after infall, whereas Sculptor and Leo I analogues stop forming stars < 2-3 Gyr after infall. Fornax analogues typically show more significant stellar mass loss and exhibit stellar tidal tails, whereas Sculptor and Leo I analogues, which are more deeply embedded in their host DM haloes at infall, do not show substantial mass loss due to tides. When additionally comparing the orbital motion of the host subaloes to the measured proper motion of Fornax we find the matching more difficult; host subhaloes tend to have pericentres smaller than that measured ones for Fornax itself. From the kinematic and orbital data, we estimate that Fornax has lost 10 − 20% of its infall stellar mass. Our best estimate for the surface brightness of a stellar tidal stream associated with Fornax is Σ ∼ 32.6 mag arcsec −2 , which may be detectable with deep imaging surveys such as DES and LSST.

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Section: Surface Densities Of Stellar Tidal Featuressupporting

confidence: 52%

Tidal features of classical Milky Way satellites in a Λ cold dark matter universe

Wang

Fattahi

Cooper

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…A diffuse stellar OD that nearly overlaps with the Phoenix stream has recently been found in the DES data (Li et al 2016). This OD (EriPhe) was previously hinted at by Carballo-Bello et al (2014) as an anomalous background population close to NGC 1261.…”

Section: Discussionmentioning

confidence: 99%

“…This feature is the EridanusPhoenix (EriPhe) OD and it is discussed in detail in a simultaneous publication (Li et al 2016). …”

Section: Search Methodsmentioning

confidence: 99%

The Phoenix Stream: A Cold Stream in the Southern Hemisphere

Balbinot¹,

Yanny²,

Li³

et al. 2016

ApJ

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We report the discovery of a stellar stream in the Dark Energy Survey Year 1 (Y1A1) data. The discovery was made through simple color-magnitude filters and visual inspection of the Y1A1 data. We refer to this new object as the Phoenix stream, after its resident constellation. After subtraction of the background stellar population we detect a clear signal of a simple stellar population. By fitting the ridge line of the stream in color-magnitude space, we find that a stellar population with age τ=11.5±0.5 Gyr and [Fe/H]<−1.6, located 17.5±0.9 kpc from the Sun, gives an adequate description of the stream stellar population. The stream is detected over an extension of 8°.1 (2.5 kpc) and has a width of ∼54 pc assuming a Gaussian profile, indicating that a globular cluster (GC) is a probable progenitor. There is no known GC within 5 kpc that is compatible with being the progenitor of the stream, assuming that the stream traces its orbit. We examined overdensities (ODs) along the stream, however, no obvious counterpart-bound stellar system is visible in the coadded images. We also find ODs along the stream that appear to be symmetrically distributed-consistent with the epicyclic OD scenario for the formation of cold streams-as well as a misalignment between the northern and southern part of stream. Despite the close proximity we find no evidence that this stream and the halo cluster NGC 1261 have a common accretion origin linked to the recently found EriPhe OD.

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“…While Turbio is detected above the background of EriPhe with a significance of s 7.9 , it would be very surprising if the two were not physically associated. It is likely that Turbio stands out more prominently in our analysis compared to that of Li et al (2016) owing to improved photometric calibration (∼0.7% vs. ∼2%), increased depth ( < g 23.5 vs. < g 22.5), and improved spatial resolution (smoothing kernel of  0 . 3 vs.  0 .…”

Section: Turbio Streammentioning

confidence: 99%

Stellar Streams Discovered in the Dark Energy Survey

Shipp

Drlica-Wagner

Balbinot

et al. 2018

ApJ

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255

254

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We perform a search for stellar streams around the Milky Way using the first 3 yr of multiband optical imaging data from the Dark Energy Survey (DES). We use DES data covering ∼5000 deg 2 to a depth of g>23.5 with a relative photometric calibration uncertainty of <1%. This data set yields unprecedented sensitivity to the stellar density field in the southern celestial hemisphere, enabling the detection of faint stellar streams to a heliocentric distance of ∼50 kpc. We search for stellar streams using a matched filter in color-magnitude space derived from a synthetic isochrone of an old, metal-poor stellar population. Our detection technique recovers four previously known thin stellar streams: Phoenix, ATLAS, Tucana III, and a possible extension of Molonglo. In addition, we report the discovery of 11 new stellar streams. In general, the new streams detected by DES are fainter, more distant, and lower surface brightness than streams detected by similar techniques in previous photometric surveys. As a by-product of our stellar stream search, we find evidence for extratidal stellar structure associated with four globular clusters: NGC 288, NGC 1261, NGC 1851, and NGC 1904. The ever-growing sample of stellar streams will provide insight into the formation of the Galactic stellar halo, the Milky Way gravitational potential, and the large-and small-scale distribution of dark matter around the Milky Way.

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Discovery of a Stellar Overdensity in Eridanus–phoenix in the Dark Energy Survey

Cited by 44 publications

References 87 publications

Tidal features of classical Milky Way satellites in a Λ cold dark matter universe

Tidal features of classical Milky Way satellites in a Λ cold dark matter universe

The Phoenix Stream: A Cold Stream in the Southern Hemisphere

Stellar Streams Discovered in the Dark Energy Survey

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