2007A&A...469..387T


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.08CET02:38:13

2007A&A...469..387T - Astronomy and Astrophysics, volume 469, 387-404 (2007/7-2)

Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds.

TISSERAND P., LE GUILLOU L., AFONSO C., ALBERT J.N., ANDERSEN J., ANSARI R., AUBOURG E., BAREYRE P., BEAULIEU J.P., CHARLOT X., COUTURES C., FERLET R., FOUQUE P., GLICENSTEIN J.F., GOLDMAN B., GOULD A., GRAFF D., GROS M., HAISSINSKI J., HAMADACHE C., DE KAT J., LASSERRE T., LESQUOY E., LOUP C., MAGNEVILLE C., MARQUETTE J.B., MAURICE E., MAURY A., MILSZTAJN A., MONIEZ M., PALANQUE-DELABROUILLE N., PERDEREAU O., RAHAL Y.R., RICH J., SPIRO M., VIDAL-MADJAR A., VIGROUX L. and ZYLBERAJCH S.

Abstract (from CDS):

The EROS-2 project was designed to test the hypothesis that massive compact halo objects (the so-called ``machos'') could be a major component of the dark matter halo of the Milky Way galaxy. To this end, EROS-2 monitored over 6.7 years 33x106 stars in the Magellanic clouds for microlensing events caused by such objects. In this work, we use only a subsample of 7x106 bright stars spread over 84deg2 of the LMC and 9deg2 of the SMC. The strategy of using only bright stars helps to discriminate against background events due to variable stars and allows a simple determination of the effects of source confusion (blending). The use of a large solid angle makes the survey relatively insensitive to effects that could make the optical depth strongly direction dependent. Using this sample of bright stars, only one candidate event was found, whereas ∼39 events would have been expected if the Halo were entirely populated by objects of mass M∼0.4M. Combined with the results of EROS-1, this implies that the optical depth toward the Large Magellanic Cloud (LMC) due to such lenses is τ<0.36x10–7 (95% CL), corresponding to a fraction of the halo mass of less than 8%. This optical depth is considerably less than that measured by the MACHO collaboration in the central region of the LMC. More generally, machos in the mass range 0.6x10–7M<M<15M are ruled out as the primary occupants of the Milky Way Halo.

Abstract Copyright:

Journal keyword(s): Galaxy: halo - cosmology: dark matter - gravitational lensing

Nomenclature: Table 2: EROS SMC N (No. 5) added, EROS LMC NN (Nos 8-12) added. Table 2, col(2): EROS2-star smNNN-Na-NNNNN N=2, EROS2-star lmNNN-Na-NNNNN N=5.

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11217 1
2 OGLE J005039.13-724154.3 Be? 00 50 39.13 -72 41 54.3   18.17 18.871 17.83 18.305 ~ 2 0
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9710 1
4 EROS2-star sm005-4m-5761 * 01 00 05.6 -72 15 03           ~ 1 0
5 MACHO 97-SMC-1 Lev 01 00 05.6 -72 15 03   18.01 17.9 18.14   ~ 25 0
6 NAME Sgr Stream St* 02 22 +00.0           ~ 683 0
7 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5868 1
8 EROS2-star lm042-1l-2622 Lev 05 01 29.2 -65 02 55           ~ 1 0
9 EROS LMC 9 Lev 05 01 29.2 -65 02 55   21.16   20.93   ~ 1 0
10 EROS2-star lm055-7m-23303 * 05 06 33.5 -71 39 45           ~ 1 0
11 EROS LMC 8 Lev 05 06 33.5 -71 39 45   21.5   20.34   ~ 3 0
12 MACHO LMC 22 Lev 05 14 32 -71 09.2     20.64     ~ 9 0
13 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15214 1
14 EROS2-star lm045-5n-26323 * 05 23 58.2 -65 52 24           ~ 1 0
15 EROS LMC 10 Lev 05 23 58.2 -65 52 24           ~ 1 0
16 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4563 2
17 EROS2-star lm061-4m-15782 * 05 53 45.4 -71 15 13           ~ 1 0
18 EROS LMC 11 Lev 05 53 45.4 -71 15 13           ~ 2 0
19 EROS LMC 12 Lev 05 59 30.0 -74 34 03           ~ 1 0
20 EROS2-star lm085-6l-14234 * 05 59 30.0 -74 34 03           ~ 1 0
21 NAME Galactic Bulge reg ~ ~           ~ 3535 0

    Equat.    Gal    SGal    Ecl

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