2022ApJ...925..118T

Query : 2022ApJ...925..118T

2022ApJ...925..118T - Astrophys. J., 925, 118-118 (2022/February-1)

From the Fire: A Deeper Look at the Phoenix Stream.

TAVANGAR K., FERGUSON P., SHIPP N., DRLICA-WAGNER A., KOPOSOV S., ERKAL D., BALBINOT E., GARCIA-BELLIDO J., KUEHN K., LEWIS G.F., LI T.S., MAU S., PACE A.B., RILEY A.H., ABBOTT T.M.C., AGUENA M., ALLAM S., ANDRADE-OLIVEIRA F., ANNIS J., BERTIN E., BROOKS D., BURKE D.L., CARNERO ROSELL A., CARRASCO KIND M., CARRETERO J., COSTANZI M., DA COSTA L.N., PEREIRA M.E.S., DE VICENTE J., DIEHL H.T., EVERETT S., FERRERO I., FLAUGHER B., FRIEMAN J., GAZTANAGA E., GERDES D.W., GRUEN D., GRUENDL R.A., GSCHWEND J., GUTIERREZ G., HINTON S.R., HOLLOWOOD D.L., HONSCHEID K., JAMES D.J., KUROPATKIN N., MAIA M.A.G., MARSHALL J.L., MENANTEAU F., MIQUEL R., MORGAN R., OGANDO R.L.C., PALMESE A., PAZ-CHINCHON F., PIERES A., PLAZAS MALAGON A.A., RODRIGUEZ-MONROY M., SANCHEZ E., SCARPINE V., SERRANO S., SEVILLA-NOARBE I., SMITH M., SUCHYTA E., SWANSON M.E.C., TARLE G., TO C., VARGA T.N., WALKER A.R. (The DES Collaboration)

Abstract (from CDS):

We use 6 yr of data from the Dark Energy Survey to perform a detailed photometric characterization of the Phoenix stellar stream, a 15° long, thin, dynamically cold, low-metallicity stellar system in the Southern Hemisphere. We use natural splines, a nonparametric modeling technique, to simultaneously fit the stream track, width, and linear density. This updated stream model allows us to improve measurements of the heliocentric distance (17.4 ± 0.1 (stat.) ±0.8 (sys.) kpc) and distance gradient (-0.009 ± 0.006 kpc deg–1) of Phoenix, which corresponds to a small change of 0.13 ± 0.09 kpc in heliocentric distance along the length of the stream. We measure linear intensity variations on degree scales, as well as deviations in the stream track on ∼2° scales, suggesting that the stream may have been disturbed during its formation and/or evolution. We recover three peaks and one gap in linear intensity along with fluctuations in the stream track. Compared to other thin streams, the Phoenix stream shows more fluctuations and, consequently, the study of Phoenix offers a unique perspective on gravitational perturbations of stellar streams. We discuss possible sources of perturbations to Phoenix, including baryonic structures in the Galaxy and dark matter subhalos.

Abstract Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Cosmology - Dark matter - Stellar streams - Galaxy structure - Astronomy data modeling - Milky Way dynamics

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 12317 1
2 NAME Phoenix Stream St* 01 35.0 -49 53           ~ 52 0
3 * alf Eri Be* 01 37 42.84548 -57 14 12.3101 -0.36 0.30 0.46 0.49 0.60 B6Vpe 495 1
4 NAME EriPhe Overdensity G 01 54 -55.0           ~ 30 0
5 NAME Aliqa Uma Stream St* 02 07 -31.5           ~ 33 0
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
7 NAME Palomar 5 Stream St* 15 16 05 -00 06.7           ~ 132 0
8 NAME GD-1 Stream St* 22 40 +31.           ~ 319 0
9 NAME ATLAS Stream St* ~ ~           ~ 44 0

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