2009A&A...501..595P


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.25CEST03:31:36

2009A&A...501..595P - Astronomy and Astrophysics, volume 501, 595-607 (2009/7-2)

Near infrared polarimetry of a sample of YSOs.

PEREYRA A., GIRART J.M., MAGALHAES A.M., RODRIGUES C.V. and DE ARAUJO F.X.

Abstract (from CDS):

Our goal is to study the physical properties of the circumstellar environment of young stellar objetcs (YSOs). In particular, the determination of the scattering mechanism can help us to constrain the optical depth of the disk and/or envelope in the near infrared. We used the IAGPOL imaging polarimeter along with the CamIV infrared camera at the LNA observatory to obtain near infrared polarimetry measurements in the H band of a sample of optically visible YSOs, namely, eleven T Tauri stars and eight Herbig Ae/Be stars. An independent determination of the disk (or jet) orientation was obtained for twelve objects from the literature. The circumstellar optical depth could then be estimated by comparing the integrated polarization position angle (PA) with the direction of the major axis of the disk projected onto the plane of the sky. Optically thin disks have, in general, a polarization PA that is perpendicular to the disk plane. In contrast, optically thick disks have polarization PAs parallel to the disks. Among the T Tauri stars, three are consistent with having optically thin disks (AS 353A, RY Tau and UY Aur) and five with optically thick disks (V536 Aql, DG Tau, DO Tau, HL Tau and LkHα 358). Among the Herbig Ae/Be stars, two stars exhibit evidence of optically thin disks (Hen 3-1191 and VV Ser) and two of optically thick disks (PDS 453 and MWC 297). Our results seem consistent with optically thick disks at near infrared bands, which are more likely to be associated with younger YSOs. Marginal evidence of polarization reversal is found in RY Tau, RY Ori, WW Vul, and UY Aur. In the first three cases, this feature can be associated with the UXOR phenomenon. Correlations with the IRAS colors and the spectral index yielded evidence of an evolutionary segregation in which the disks tend to be optically thin when they are older.

Abstract Copyright:

Journal keyword(s): polarization - infrared: stars - stars: pre-main sequence - circumstellar matter

Simbad objects: 31

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Number of rows : 31

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 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 650 1
2 V* T Tau Or* 04 21 59.4323326335 +19 32 06.439974179   11.01 9.30 9.80   K0IV/Ve 1253 2
3 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 930 1
4 EM* LkHA 358 TT* 04 31 36.1396524070 +18 13 43.176961457     19.0     M0.9 87 0
5 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1219 0
6 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
7 V* DO Tau Or* 04 38 28.5882167490 +26 10 49.472067634 12.78 13.44 12.30 13.01   M1Ve 318 1
8 V* UY Aur Or* 04 51 47.3900418279 +30 47 13.552212742 12.82 12.96 11.90 10.59 9.52 M0e+M2.5e 329 0
9 V* SU Aur Or* 04 55 59.3861369488 +30 34 01.499800471   10.33 9.30 9.17   G2IIIne 535 0
10 V* UX Ori Ae* 05 04 29.9881676817 -03 47 14.288047238 10.25 10.93 8.70 9.62 9.43 A4IVe 334 1
11 V* CO Ori Or* 05 27 38.3352 +11 25 38.923 12.96 12.33 10.30 10.33 9.63 F7Ve 155 0
12 V* RY Ori Or* 05 32 09.9419985443 -02 49 46.769539985 12.62 12.76 10.80 10.82 10.34 F7 49 0
13 IC 446 Cl* 06 31 02.3 +10 26 06           ~ 50 1
14 V* VY Mon Ae* 06 31 06.9180562526 +10 26 04.982093681 16.65 15.45 13.70 12.49 11.00 A5:Vep 87 0
15 IRAS 06283+1028 mul 06 31 07.0 +10 26 05           ~ 44 1
16 GSC 07855-00815 * 16 05 03.9081582025 -39 45 03.767552355   14.54 13.93     A5V 13 0
17 Haro 1-1 Or* 16 21 34.7046243951 -26 12 26.914958774   14.59       K5e 57 0
18 WRAY 15-1484 Em* 16 27 15.1095981539 -48 39 26.849684049   14.6 13.7     B[e] 52 0
19 LDN 1767 DNe 17 18.6 -26 45           ~ 4 0
20 IRAS 17178-2600 Ae? 17 20 56.1332742391 -26 03 30.559251464   13.7 12.92     F2V 15 0
21 EM* MWC 297 Ae* 18 27 39.5266257570 -03 49 52.136526892 15.57 14.34 12.31 11.34   B1.5Ve 266 0
22 V* VV Ser Ae* 18 28 47.8619658319 +00 08 39.924642619 12.99 12.63 11.80 11.01 10.24 A5Ve 228 0
23 IRAS 18275+0040 Y*O 18 30 06.1724662068 +00 42 33.550675181   17.27 15.55 13.34   F3Ve 18 0
24 HH 32A HH 19 20 29.49 +11 02 01.7           ~ 38 0
25 HH 32B HH 19 20 29.77 +11 01 57.2           ~ 20 0
26 EM* AS 353 Or* 19 20 30.9919486938 +11 01 54.604157558   13.22 12.21     K5 180 1
27 HH 32D HH 19 20 31.29 +11 01 50.5           ~ 13 0
28 HH 32C HH 19 20 31.3 +11 01 51           ~ 17 0
29 V* WW Vul Ae* 19 25 58.7494596284 +21 12 31.333220807 11.46 10.99 10.25 10.38 10.12 A2IVe 214 0
30 V* PX Vul Or* 19 26 40.2533631097 +23 53 50.777553057 12.56 12.57 11.83 10.90 10.30 F3Ve 49 0
31 V* V536 Aql Or* 19 38 57.413016 +10 30 15.99804     14.85 12.27   KV:e 58 0

    Equat.    Gal    SGal    Ecl

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2020.09.25-03:31:36

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