2020ApJ...893...48N

Query : 2020ApJ...893...48N

2020ApJ...893...48N - Astrophys. J., 893, 48-48 (2020/April-2)

Milky Way satellite census. II. Galaxy-halo connection constraints including the impact of the Large Magellanic Cloud.

NADLER E.O., WECHSLER R.H., BECHTOL K., MAO Y.-Y., GREEN G., DRLICA-WAGNER A., McNANNA M., MAU S., PACE A.B., SIMON J.D., KRAVTSOV A., DODELSON S., LI T.S., RILEY A.H., WANG M.Y., ABBOTT T.M.C., AGUENA M., ALLAM S., ANNIS J., AVILA S., BERNSTEIN G.M., BERTIN E., BROOKS D., BURKE D.L., CARNERO ROSELL A., CARRASCO KIND M., CARRETERO J., COSTANZI M., DA COSTA L.N., DE VICENTE J., DESAI S., EVRARD A.E., FLAUGHER B., FOSALBA P., FRIEMAN J., GARCIA-BELLIDO J., GAZTANAGA E., GERDES D.W., GRUEN D., GSCHWEND J., GUTIERREZ G., HARTLEY W.G., HINTON S.R., HONSCHEID K., KRAUSE E., KUEHN K., KUROPATKIN N., LAHAV O., MAIA M.A.G., MARSHALL J.L., MENANTEAU F., MIQUEL R., PALMESE A., PAZ-CHINCHON F., PLAZAS A.A., ROMER A.K., SANCHEZ E., SANTIAGO B., SCARPINE V., SERRANO S., SMITH M., SOARES-SANTOS M., SUCHYTA E., TARLE G., THOMAS D., VARGA T.N., WALKER A.R. (The DES Collaboration)

Abstract (from CDS):

The population of Milky Way (MW) satellites contains the faintest known galaxies and thus provides essential insight into galaxy formation and dark matter microphysics. Here we combine a model of the galaxy-halo connection with newly derived observational selection functions based on searches for satellites in photometric surveys over nearly the entire high Galactic latitude sky. In particular, we use cosmological zoom-in simulations of MW-like halos that include realistic Large Magellanic Cloud (LMC) analogs to fit the position-dependent MW satellite luminosity function. We report decisive evidence for the statistical impact of the LMC on the MW satellite population due to an estimated 6 ± 2 observed LMC-associated satellites, consistent with the number of LMC satellites inferred from Gaia proper-motion measurements, confirming the predictions of cold dark matter models for the existence of satellites within satellite halos. Moreover, we infer that the LMC fell into the MW within the last 2 Gyr at high confidence. Based on our detailed full-sky modeling, we find that the faintest observed satellites inhabit halos with peak virial masses below 3.2×108 M☉ at 95% confidence, and we place the first robust constraints on the fraction of halos that host galaxies in this regime. We predict that the faintest detectable satellites occupy halos with peak virial masses above 106 M☉, highlighting the potential for powerful galaxy formation and dark matter constraints from future dwarf galaxy searches.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Dark matter - Milky Way dark matter halo - Galaxy abundances

Simbad objects: 43

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Number of rows : 43
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 Tuc IV G 00 02.9 -60 51           ~ 90 0
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 12317 1
3 NAME Sculptor Dwarf Galaxy G 01 00 09.4 -33 42 32   9.79 8.6 8.81   ~ 1498 4
4 NAME Cetus II G 01 17.9 -17 25           ~ 56 0
5 NAME Tri II G 02 13 17.40 +36 10 42.4           ~ 164 0
6 NAME Segue 2 G 02 19 16.0 +20 10 31     15.2     ~ 299 0
7 MCG-06-07-001 G 02 39 59.3 -34 26 57   9.02 7.4     ~ 1894 1
8 NAME Hor I G 02 55 31.7 -54 07 08           ~ 169 0
9 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7988 0
10 NAME Horologium II G 03 16 32.1 -50 01 05           ~ 76 0
11 NAME Reticulum II G 03 35 42.1 -54 02 57           ~ 375 0
12 NAME Eridanus II G 03 44 21.1 -43 32 00           ~ 216 0
13 NAME Reticulum III G 03 45.4 -60 27           ~ 67 0
14 NAME Pic I G 04 43 47.4 -50 16 59           ~ 58 0
15 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
16 NAME Col I G 05 31.4 -28 02           ~ 60 0
17 NAME UMa II Galaxy G 08 51 30.0 +63 07 48     13.3     ~ 410 0
18 NAME Segue 1 G 10 07 03.2 +16 04 25     15.3     ~ 517 1
19 Z 64-73 G 10 08 28.12 +12 18 23.4   11.3 10.0     ~ 1284 1
20 NAME Sextans dSph LSB 10 13 02.9 -01 36 53   12 10.4     ~ 921 0
21 NAME Willman 1 G 10 49 21.0 +51 03 00     15.2     ~ 345 0
22 Z 126-111 G 11 13 28.13 +22 09 10.1   12.9 12.0     ~ 899 0
23 NAME Leo IV LSB 11 32 57.0 -00 32 00     15.1     ~ 419 1
24 NAME Crater Cluster GlC 11 36 16.20 -10 52 38.8           ~ 117 1
25 NAME Crater II Dwarf Galaxy G 11 49 14 -18 24.8           ~ 176 0
26 NAME Coma Dwarf Galaxy G 12 26 59.0 +23 54 15     14.1     ~ 482 1
27 NAME CVn II dSph G 12 57 09.6 +34 19 12     16.1     ~ 287 2
28 NAME CVn I dSph G 13 28 03.5 +33 33 21     13.1     ~ 352 1
29 NAME Bootes Dwarf Spheroidal Galaxy G 14 00 00.0 +14 30 00     12.8     ~ 491 0
30 Z 318-18 G 15 09 08.0 +67 13 21   13.60 10.6     ~ 1459 0
31 NAME Draco II Gl? 15 52 47.6 +64 33 55           ~ 138 0
32 NAME Hercules Dwarf Galaxy G 16 31 02.0 +12 47 30     14.0     ~ 379 1
33 Z 300-12 G 17 20 14.335 +57 55 16.39   12.40 10.6     ~ 1428 1
34 NAME Sagittarius II Gl? 19 52 40.5 -22 04 05           ~ 97 0
35 NAME Indus I Cl* 21 08 49.970 -51 09 48.60           ~ 68 0
36 NAME Gru II G 22 04.1 -46 26           ~ 110 0
37 NAME Tuc II G 22 51 55.1 -58 34 08           ~ 192 0
38 NAME Grus I G 22 56 42.4 -50 09 48           ~ 126 0
39 NAME Tuc V G 23 37.4 -63 16           ~ 84 0
40 NAME Phe II G 23 39 59.4 -54 24 22           ~ 107 0
41 NAME Tuc III G 23 56.6 -59 36           ~ 229 0
42 NAME Gaia Enceladus-Sausage St* ~ ~           ~ 860 0
43 NAME Local Group GrG ~ ~           ~ 9325 0

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