Back to Search Start Over

Two Ultra-faint Milky Way Stellar Systems Discovered in Early Data from the DECam Local Volume Exploration Survey

Authors :
Erik Tollerud
L. C. Johnson
D. Hernandez-Lang
Steven R. Majewski
Guy S. Stringfellow
David J. Sand
M. McNanna
Keith Bechtol
J. D. Simon
C. E. Martínez-Vázquez
Yao-Yuan Mao
N. P. Kuropatkin
Alistair R. Walker
David James
Eric H. Neilsen
Prashin Jethwa
Marcelle Soares-Santos
Brian Yanny
Risa H. Wechsler
Andrew B. Pace
R. P. van der Marel
Y. Choi
Adriano Pieres
Sahar S. Allam
Allison K. Hughes
Pol Massana
Eric F. Bell
Denis Erkal
S. Mau
Jeffrey L. Carlin
F. Paz-Chinchón
Wayne A. Barkhouse
Knut Olsen
P. S. Ferguson
Burçin Mutlu-Pakdil
Monika Adamów
Tenglin Li
David L. Nidever
A. Zenteno
P. Balaji
Eric Morganson
K. Tavangar
Carme Gallart
Ethan O. Nadler
Kyler Kuehn
Noelia E. D. Noël
Alex Drlica-Wagner
Javier Sanchez
Denija Crnojević
L. Santana-Silva
A. H. Riley
W. Cerny
Antonella Palmese
Douglas L. Tucker
Nora Shipp
Antonela Monachesi
A. K. Vivas
J. Esteves
Robert A. Gruendl
Source :
The Astrophysical Journal. 890:136
Publication Year :
2020
Publisher :
American Astronomical Society, 2020.

Abstract

We report the discovery of two ultra-faint stellar systems found in early data from the DECam Local Volume Exploration survey (DELVE). The first system, Centaurus I (DELVE J1238-4054), is identified as a resolved overdensity of old and metal-poor stars with a heliocentric distance of ${\rm D}_{\odot} = 116.3_{-0.6}^{+0.6}$ kpc, a half-light radius of $r_h = 2.3_{-0.3}^{+0.4}$ arcmin, an age of $\tau > 12.85$ Gyr, a metallicity of $Z = 0.0002_{-0.0002}^{+0.0001}$, and an absolute magnitude of $M_V = -5.55_{-0.11}^{+0.11}$ mag. This characterization is consistent with the population of ultra-faint satellites, and confirmation of this system would make Centaurus I one of the brightest recently discovered ultra-faint dwarf galaxies. Centaurus I is detected in Gaia DR2 with a clear and distinct proper motion signal, confirming that it is a real association of stars distinct from the Milky Way foreground; this is further supported by the clustering of blue horizontal branch stars near the centroid of the system. The second system, DELVE 1 (DELVE J1630-0058), is identified as a resolved overdensity of stars with a heliocentric distance of ${\rm D}_{\odot} = 19.0_{-0.6}^{+0.5} kpc$, a half-light radius of $r_h = 0.97_{-0.17}^{+0.24}$ arcmin, an age of $\tau = 12.5_{-0.7}^{+1.0}$ Gyr, a metallicity of $Z = 0.0005_{-0.0001}^{+0.0002}$, and an absolute magnitude of $M_V = -0.2_{-0.6}^{+0.8}$ mag, consistent with the known population of faint halo star clusters. Given the low number of probable member stars at magnitudes accessible with Gaia DR2, a proper motion signal for DELVE 1 is only marginally detected. We compare the spatial position and proper motion of both Centaurus I and DELVE 1 with simulations of the accreted satellite population of the Large Magellanic Cloud (LMC) and find that neither is likely to be associated with the LMC.<br />Comment: 17 pages, 6 figures, 1 table; updated to match published version; updated to address erratum

Details

ISSN :
15384357 and 12384054
Volume :
890
Database :
OpenAIRE
Journal :
The Astrophysical Journal
Accession number :
edsair.doi.dedup.....9b71d02dba673ad180d4c95d0b025818
Full Text :
https://doi.org/10.3847/1538-4357/ab6c67