2011MNRAS.415.1138P


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.28CET10:58:40

2011MNRAS.415.1138P - Mon. Not. R. Astron. Soc., 415, 1138-1154 (2011/August-1)

Chemically tagging the Hyades stream: does it partly originate from the Hyades cluster?

POMPEIA L., MASSERON T., FAMAEY B., VAN ECK S., JORISSEN A., MINCHEV I., SIEBERT A., SNEDEN C., LEPINE J.R.D., SIOPIS C., GENTILE G., DERMINE T., PASQUATO E., VAN WINCKEL H., WAELKENS C., RASKIN G., PRINS S., PESSEMIER W., HENSBERGE H., FREMAT Y., DUMORTIER L. and BIENAYME O.

Abstract (from CDS):

The Hyades stream has long been thought to be a dispersed vestige of the Hyades cluster. However, recent analyses of the parallax distribution, of the mass function, and of the action-space distribution of stream stars have shown it to be rather composed of orbits trapped at a resonance of a density disturbance. This resonant scenario should leave a clearly different signature in the element abundances of stream stars than the dispersed cluster scenario, since the Hyades cluster is chemically homogeneous. Here, we study the metallicity as well as the element abundances of Li, Na, Mg, Fe, Zr, Ba, La, Ce, Nd and Eu for a random sample of stars belonging to the Hyades stream, and compare them with those of stars from the Hyades cluster. From this analysis: (i) we independently confirm that the Hyades stream cannot be solely composed of stars originating in the Hyades cluster; (ii) we show that some stars (namely 2/21) from the Hyades stream nevertheless have abundances compatible with an origin in the cluster; (iii) we emphasize that the use of Li as a chemical tag of the cluster origin of main-sequence stars is very efficient in the range 5500 K ≤ Teff ≤ 6200 K, since the Li sequence in the Hyades cluster is very tight, while at the same time spanning a large abundance range; (iv) we show that, while this evaporated population has a metallicity excess of ∼0.2 dex with respect to the local thin-disc population, identical to that of the Hyades cluster, the remainder of the Hyades stream population has still a metallicity excess of ∼0.06-0.15 dex, consistent with an origin in the inner Galaxy and (v) we show that the Hyades stream can be interpreted as an inner 4:1 resonance of the spiral pattern: this then also reproduces an orbital family compatible with the Sirius stream, and places the origin of the Hyades stream up to 1 kpc inwards from the solar radius, which might explain the observed metallicity excess of the stream population.

Based on observations obtained with the HERMES/Mercator spectrograph/telescope installed at the Roque de los Muchachos Observatory, La Palma, Spain.


Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS

Journal keyword(s): Galaxy: evolution - Galaxy: kinematics and dynamics - open clusters and associations: individual: Hyades

Simbad objects: 38

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Number of rows : 38

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 BD+17 455 PM* 02 55 16.2855708047 +17 53 30.157855318   9.52 8.80     K0 20 0
2 V* BW Ari BY* 02 57 46.6726058921 +29 39 41.266403609 10.24 9.778   8.10   K0V 67 0
3 V* BZ Cet BY* 03 00 02.8120517172 +07 44 59.117432323 9.635 8.908 7.955 7.436 6.994 K2.5Vk 109 0
4 HD 19902 BY* 03 13 02.7936218426 +32 53 47.216461927   8.892   7.7   G5V 54 0
5 HD 20430 ** 03 17 26.3862804449 +07 39 20.918381490   7.958 7.373 7.050 6.739 F8 120 0
6 HD 20439 PM* 03 17 32.7801660070 +07 41 24.555463939   8.376 7.747 7.402 7.085 ~ 118 0
7 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2928 0
8 * 39 Tau ** 04 05 20.2584363613 +22 00 32.055953585   6.52   5.5   G5V 198 0
9 HD 26257 PM* 04 09 09.0703834146 +00 10 44.300862057   8.17 7.63     G2V 38 0
10 HD 26756 PM* 04 14 25.6502208510 +14 37 30.119616339   9.125 8.419 8.039 7.682 G5V 177 0
11 V* V1309 Tau BY* 04 14 27.2545515447 +12 26 07.132723657   8.682 8.030 7.673 7.341 G0 142 0
12 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2607 0
13 HD 42132 * 06 08 47.7018467671 -06 49 16.937932718   7.34 6.46     G8III/IV 19 0
14 HD 67827 PM* 08 11 21.6509382830 +38 43 52.729347036   7.188 6.597     G0 45 0
15 HD 86165 PM* 09 58 15.7070374411 +51 34 08.131421496       7.6   G0 22 0
16 HD 89793 PM* 10 22 10.0519118214 +16 28 11.513629006   9.54 8.80     G5 27 0
17 HD 90936 PM* 10 29 33.4293481131 -18 14 38.016543803   8.99 8.36     G3V 32 0
18 HD 103891 PM* 11 57 45.3028703143 -08 32 55.365134769   9.078 8.646     F8V 52 0
19 HD 108351 PM* 12 27 02.5194619812 -22 23 22.679365200   8.43 7.88     F7V 26 0
20 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 373 2
21 HD 133430 PM* 14 59 05.8256297773 +73 25 33.328375378   9.17 8.54     G5 20 0
22 HD 134694 PM* 15 10 25.6736773993 +25 26 41.490279139   8.92 8.47     F8 20 0
23 HD 142072 Ro* 15 52 33.7494008456 -01 54 22.782518327   8.53 7.878   7.131 G6V 37 0
24 HD 149028 PM* 16 31 37.0744122593 +12 25 17.569691453   9.23 8.49     GV 29 0
25 HD 149285 * 16 33 19.3745399871 +15 08 18.342257780   9.30 8.81     G5 15 0
26 HD 151766 * 16 48 42.7254282708 +18 19 08.135217694   8.13 7.60     F8 16 0
27 HD 155968 PM* 17 14 58.0721875815 -02 30 11.325930564   9.08 8.40     G3V 38 0
28 HD 157347 PM* 17 22 51.2877095327 -02 23 17.439826176   6.965 6.278     G3V 156 0
29 HD 162808 * 17 52 25.5938275077 +11 59 28.922592166   8.99 8.40     G5 23 0
30 HD 171067 PM* 18 32 10.4644644449 +13 44 11.631045018       6.8   G6V 64 0
31 HD 180712 PM* 19 14 01.4612679932 +59 33 06.561652145   8.57 7.99     F8 18 0
32 HD 187237 PM* 19 48 00.8812665154 +27 52 10.303035275   7.51   6.5   G2IV-V 65 0
33 HD 189087 PM* 19 57 13.4148800901 +29 49 26.455056667   8.68   7.4   G8 77 0
34 NAME Hercules Stream MGr ~ ~           ~ 174 0
35 NAME Sirius Moving Group MGr ~ ~           ~ 74 0
36 NAME HR 1614 Moving Group As* ~ ~           ~ 40 0
37 NAME Galactic Bar reg ~ ~           ~ 846 0
38 NAME Hyades Moving Group MGr ~ ~           ~ 232 1

    Equat.    Gal    SGal    Ecl

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2020.01.28-10:58:40

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