2010ApJ...725.1100G


Query : 2010ApJ...725.1100G

2010ApJ...725.1100G - Astrophys. J., 725, 1100-1110 (2010/December-2)

Near-IR H2 emission of protostars: probing circumstellar environments.

GREENE T.P., BARSONY M. and WEINTRAUB D.A.

Abstract (from CDS):

We present new observations of near-infrared molecular hydrogen (H2) line emission in a sample of 18 Class I and flat-spectrum low-mass protostars, primarily in the Tau-Aur and ρ Oph dark clouds. The line emission is extended by up to several arcseconds (several hundred AU) for most objects, and there is little night-to-night variation in line strength coincident with the continuum point source. Flux ratios of H2 v = 2-1 S(1) and v = 1-0 S(1) lines are consistent with this emission arising in jets or winds in many objects. However, most objects have only small offsets (under 10 km/s) between their H2 and photospheric radial velocities. No objects have line ratios which are clearly caused solely by UV excitation, but the H2emission of several objects may be caused by UV or X-ray excitation in the presence of circumstellar dust. There are several objects in the sample whose observed velocities and line fluxes suggest quiescent, non-mechanical origins for their molecular hydrogen emissions. Overall, we find the H2 emission properties of these protostars to be similar to the T Tauri stars studied in previous surveys.

Abstract Copyright:

Journal keyword(s): infrared: stars - ISM: jets and outflows - stars: formation - stars: pre-main sequence - techniques: spectroscopic

Simbad objects: 29

goto Full paper

goto View the references in ADS

Number of rows : 29
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 HD 20165 PM* 03 14 47.2271488882 +08 58 50.857104978 9.278 8.68 7.800 7.319 6.895 K1V 109 0
2 [LAL96] 213 Y*O 03 29 07.739 +31 21 57.52           ~ 52 0
3 IRAS 03260+3111 mul 03 29 10.4 +31 21 59           ~ 14 0
4 NAME IRAS 04108+2803B Y*O 04 13 54.71688 +28 11 32.8992           K0-M3 37 0
5 IRAS 04158+2805 Y*O 04 18 58.1407377664 +28 12 23.347645825           M5.25 91 0
6 IRAS 04181+2654 Y*O 04 21 11.46888 +27 01 09.4044           G0-M3 60 0
7 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 967 1
8 HD 28343 Er* 04 29 00.1237376701 +21 55 21.719015238 10.988 9.688 8.300 7.446 6.656 M0.5V 170 0
9 HD 28354 ** 04 29 19.8323301686 +27 24 15.190536329   6.519 6.548     B9Vn 32 0
10 IRAS 04264+2433 Y*O 04 29 30.08016 +24 39 55.0548   18.40   16.73 14.67 ~ 39 0
11 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1264 0
12 IRAS 04295+2251 Y*O 04 32 32.05488 +22 57 26.6724           K0-M4 89 0
13 IRAS 04361+2547 Y*O 04 39 13.89288 +25 53 20.8788           ~ 189 1
14 IRAS 04365+2535 Y*O 04 39 35.19360 +25 41 44.7252           ~ 252 0
15 HD 285968 PM* 04 42 55.7753203198 +18 57 29.394344631 12.668 11.49 9.951 8.931 7.702 M2.5V 277 2
16 * ome Sco bC* 16 06 48.4269211 -20 40 09.090235 3.10 3.92 3.97 3.91 3.99 B1V 447 0
17 * d Sco PM* 16 18 17.9001656 -28 36 50.476788   4.804 4.782     A1Va 152 0
18 * rho Oph ** 16 25 35.11766 -23 26 49.8150 4.30 4.85 4.63 4.27 3.96 B2IV+B2V 625 0
19 GSS 30 Y*O 16 26 21.38160 -24 23 04.0524           ~ 205 1
20 [GY92] 21 Y*O 16 26 23.57976 -24 24 39.4956           K7 65 2
21 VSSG 30 Y*O 16 26 44.19504 -24 34 48.3492           ~ 130 0
22 WL 6 Y*O 16 27 21.80448 -24 29 53.3616           ~ 113 0
23 YLW 15 Y*O 16 27 26.93640 -24 40 50.8224           ~ 246 1
24 YLW 16A Y*O 16 27 28.02744 -24 39 33.5052           K8 187 0
25 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3227 1
26 WLY 2-67 Y*O 16 32 00.99624 -24 56 41.9640           ~ 56 0
27 HD 168966 SB* 18 22 26.9586166366 -00 44 51.134284288   9.22 8.88     A0V 5 0
28 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 986 2
29 V* WY Cas S* 23 58 01.3075303591 +56 29 13.468672815   12.48 10.76     S6-6.5/6-e 71 0

To bookmark this query, right click on this link: simbad:objects in 2010ApJ...725.1100G and select 'bookmark this link' or equivalent in the popup menu


2021.10.20-19:54:06

© Université de Strasbourg/CNRS

    • Contact