2000AJ....120.1426G


Query : 2000AJ....120.1426G

2000AJ....120.1426G - Astron. J., 120, 1426-1435 (2000/September-0)

Chandra X-ray observatory study of the Orion nebula cluster and BN/KL region.

GARMIRE G., FEIGELSON E.D., BROOS P., HILLENBRAND L.A., PRAVDO S.H., TOWNSLEY L. and TSUBOI Y.

Abstract (from CDS):

About 1000 X-ray emitting young pre-main-sequence (PMS) stars distributed in mass from ∼0.05 M brown dwarfs to a ∼50 M O star are detected in an image of the Orion Nebula obtained with the Advanced CCD Imaging Spectrometer on board the Chandra X-Ray Observatory. This is the richest field of sources ever obtained in X-ray astronomy. Individual X-ray luminosities in the Orion Nebula cluster range from the sensitivity limit of 2x1028 ergs.s–1 to ∼1032 ergs.s–1. ACIS sources include 85%-90% of V<20 stars, plus a lower but substantial fraction of deeply embedded stars with extinctions as high as AV≃60. The relationships between X-ray and other PMS stellar properties suggest that X-ray luminosity of lower-mass PMS stars depends more on mass, and possibly stellar rotation, than on bolometric luminosity, as widely reported. In a subsample of 17 unabsorbed stars with mass ≃1 M, X-ray luminosities are constant at a high level around Lx≃2x1030 ergs.s–1 for the first ≃2 Myr while descending the convective Hayashi track, but diverge during the 2-10 Myr phase with X-ray emission plummeting in some stars but remaining high in others. This behavior is consistent with the distribution of X-ray luminosities on the zero-age main sequence and with current theories of their rotational history and magnetic dynamos.

The sources in the Becklin-Neugebauer/Kleinman-Low region of massive star formation are discussed in detail. They include both unabsorbed and embedded low-mass members of the Orion Nebula cluster, the luminous infrared Source n, and a class of sources without optical or infrared counterparts that may be new magnetically active embedded PMS stars. Several X-ray sources are also variable radio emitters, an association often seen in magnetically active PMS stars. Faint X-ray emission is seen close to, but apparently not coincident with, the Becklin-Neugebauer object. Its nature is not clear.


Abstract Copyright:

Journal keyword(s): Infrared Radiation - ISM: Individual: Name: Orion Nebula - Stars: Activity - Stars: Pre-Main-Sequence - X-Rays

VizieR on-line data: <Available at CDS (J/AJ/120/1426): table1.dat table2.dat notes.dat>

Nomenclature: Table 1: [GFB2000] ONC NNN (Nos 1-973) = CXOONC JHHMMSS.s+DDMMSS N=973. Table 2: [GFB2000] BN NN (Nos 1-27) = CXOONC JHHMMSS.s+DDMMSS N=27.

Status at CDS : All or part of tables of objects could be ingested in SIMBAD with priority 2.

CDS comments: Infrared source n = LBLS n, source radio D = GMR D

Simbad objects: 20

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Number of rows : 20
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 Cl Melotte 22 OpC 03 46 24 +24 06.8           ~ 3208 0
2 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2160 1
3 V* V2154 Ori Or* 05 35 05.4544440312 -05 22 30.491842116         16.344 M6.5 32 0
4 COUP 590 * 05 35 13.9700 -05 22 31.900           ~ 55 0
5 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1112 2
6 COUP 600 * 05 35 14.0858526024 -05 22 36.519966912     15.906   12.799 M3 50 0
7 V* V2254 Ori Or* 05 35 14.11296 -05 22 22.7316           B 304 2
8 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2167 1
9 [GD77] A IR 05 35 14.19 -05 22 34.0           ~ 62 0
10 MLLA 610 IR 05 35 14.278 -05 22 30.65           ~ 74 0
11 COUP 621 Y*O 05 35 14.35371 -05 22 32.8820           ~ 106 0
12 [RLK73] IRc 2 IR 05 35 14.51548 -05 22 30.5943           ~ 609 1
13 COUP 662 * 05 35 14.8982780 -05 22 25.410079           ~ 37 0
14 MLLA 606 Y*O 05 35 15.030 -05 22 31.15         15.161 M6 29 0
15 V* V1331 Ori Y*O 05 35 15.3447031560 -05 22 15.575087208   15.777 14.474   11.707 K3e 56 0
16 CXOONC J053515.8-052431 * 05 35 15.89714 -05 24 31.0774           M5.5-M7 13 0
17 * tet01 Ori C SB* 05 35 16.4662967280 -05 23 22.921811880 4.20 5.15 5.13 4.91 4.73 O7Vp 1351 1
18 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1549 1
19 M 42 HII 05 35 17.3 -05 23 28           ~ 3919 0
20 CXOONC J053518.2-052346 * 05 35 18.210 -05 23 46.30           ~ 16 0

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2022.08.14-11:07:46

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