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


Query : 2009A&A...501..595P

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 - 2023
#notes
1 V* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 684 1
2 V* T Tau TT* 04 21 59.4319873992 +19 32 06.432393336   11.22 10.12 9.80   K0IV/Ve 1373 1
3 V* DG Tau Or* 04 27 04.6921275888 +26 06 16.060169268 13.57 13.97 10.50 12.28   K6Ve 1000 1
4 EM* LkHA 358 TT* 04 31 36.1433863008 +18 13 43.204853460     19.0     M0.9 92 0
5 V* HL Tau Or* 04 31 38.5107609312 +18 13 57.859747968   15.89 14.49 14.39   K5 1360 0
6 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
7 V* DO Tau Or* 04 38 28.5880527336 +26 10 49.467596196 12.78 13.44 12.30 13.01   M1Ve 348 1
8 V* UY Aur Or* 04 51 47.3890167432 +30 47 13.551561492 12.82 12.96 11.90 10.59 9.52 M0e+M2.5e 347 0
9 V* SU Aur Or* 04 55 59.3866872552 +30 34 01.499608092   10.33 9.30 9.17   G2IIIne 574 0
10 V* UX Ori Ae* 05 04 29.9878898040 -03 47 14.286732072 10.25 10.93 8.70 9.62 9.43 A4IVe 354 1
11 V* CO Ori Or* 05 27 38.3386648 +11 25 38.974625 12.96 12.33 10.30 10.33 9.63 F7Ve 162 0
12 V* RY Ori Or* 05 32 09.9419233368 -02 49 46.770599784 12.62 12.76 10.80 10.82 10.34 F7 57 0
13 IC 446 Cl* 06 31 02.3 +10 26 06           ~ 58 1
14 V* VY Mon Ae* 06 31 06.9271406952 +10 26 04.952351076 16.65 15.45 13.70 12.49 11.00 A5:Vep 93 0
15 IRAS 06283+1028 mul 06 31 07.0 +10 26 05           ~ 44 1
16 GSC 07855-00815 * 16 05 03.9087521832 -39 45 03.780324972   14.54 13.93     A5V 13 0
17 Haro 1-1 Or* 16 21 34.7045923320 -26 12 26.913018060   14.59       K5e 59 0
18 WRAY 15-1484 Em* 16 27 15.1097295456 -48 39 26.852709060   14.706 13.782 13.388   B[e] 55 0
19 LDN 1767 DNe 17 18.6 -26 45           ~ 4 0
20 IRAS 17178-2600 PN? 17 20 56.1353525664 -26 03 30.577658436   14.408 13.627 12.879   F2Ve 16 0
21 EM* MWC 297 Ae* 18 27 39.5265500160 -03 49 52.133050776 15.57 14.34 12.31 11.34   B1.5Ve 286 0
22 V* VV Ser Ae* 18 28 47.8620017808 +00 08 39.923474964 12.99 12.63 11.80 11.01 10.24 A5Ve 242 0
23 IRAS 18275+0040 Y*O 18 30 06.1720554216 +00 42 33.552210636   17.27 15.55 13.34   F3Ve 23 0
24 HH 32A HH 19 20 29.49 +11 02 01.7           ~ 39 0
25 HH 32B HH 19 20 29.77 +11 01 57.2           ~ 21 0
26 EM* AS 353 Or* 19 20 30.9918166680 +11 01 54.605482968   13.22 12.21     K5 186 1
27 HH 32D HH 19 20 31.29 +11 01 50.5           ~ 14 0
28 HH 32C HH 19 20 31.3 +11 01 51           ~ 17 0
29 V* WW Vul Ae* 19 25 58.7494120560 +21 12 31.333658616 11.46 10.99 10.25 10.38 10.12 A2IVe 221 0
30 V* PX Vul Or* 19 26 40.2532914312 +23 53 50.782579116 12.56 12.57 11.83 10.90 10.30 F3Ve 53 0
31 V* V536 Aql Or* 19 38 57.413016 +10 30 15.99804     14.85 12.27   KV:e 59 0

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2023.02.06-00:44:02

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