2015ApJ...804..143H


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.18CET05:17:10

2015ApJ...804..143H - Astrophys. J., 804, 143 (2015/May-2)

High-resolution 25 M imaging of the disks around Herbig Ae/Be stars.

HONDA M., MAASKANT K., OKAMOTO Y.K., KATAZA H., YAMASHITA T., MIYATA T., SAKO S., FUJIYOSHI T., SAKON I., FUJIWARA H., KAMIZUKA T., MULDERS G.D., LOPEZ-RODRIGUEZ E., PACKHAM C. and ONAKA T.

Abstract (from CDS):

We imaged circumstellar disks around 22 Herbig Ae/Be stars at 25 µm using Subaru/COMICS and Gemini/T-ReCS. Our sample consists of an equal number of objects from each of the two categories defined by Meeus et al.; 11 group I (flaring disk) and II (flat disk) sources. We find that group I sources tend to show more extended emission than group II sources. Previous studies have shown that the continuous disk is difficult to resolve with 8 m class telescopes in the Q band due to the strong emission from the unresolved innermost region of the disk. This indicates that the resolved Q-band sources require a hole or gap in the disk material distribution to suppress the contribution from the innermost region of the disk. As many group I sources are resolved at 25 µm, we suggest that many, but not all, group I Herbig Ae/Be disks have a hole or gap and are (pre-)transitional disks. On the other hand, the unresolved nature of many group II sources at 25 µm supports the idea that group II disks have a continuous flat disk geometry. It has been inferred that group I disks may evolve into group II through the settling of dust grains into the mid-plane of the protoplanetary disk. However, considering the growing evidence for the presence of a hole or gap in the disk of group I sources, such an evolutionary scenario is unlikely. The difference between groups I and II may reflect different evolutionary pathways of protoplanetary disks.

Abstract Copyright:

Journal keyword(s): circumstellar matter - protoplanetary disks - stars: pre-main sequence

Simbad objects: 33

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Number of rows : 33

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 * bet And PM* 01 09 43.92388 +35 37 14.0075 5.58 3.62 2.05 0.81 -0.19 M0+IIIa 531 0
2 V* V892 Tau Ae* 04 18 40.6120892867 +28 19 15.641672501   16.6 14.69 14.35   A0Ve 259 1
3 * alf Tau LP? 04 35 55.23907 +16 30 33.4885 4.32 2.40 0.86 -0.37 -1.31 K5+III 1176 1
4 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 913 2
5 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 383 0
6 HD 35187 Y*O 05 24 01.17261 +24 57 37.5791   8.79 8.71 8.72   A2e+A7 93 0
7 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 337 0
8 V* CQ Tau Ae* 05 35 58.4671238887 +24 44 54.086375712 11.290 10.780 10.000   8.33 F5IVe 250 0
9 HD 97048 Ae* 11 08 03.3105687971 -77 39 17.491180130 9.03 8.76 9.00   8.64 A0Vep 446 0
10 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 632 1
11 * gam Cru PM* 12 31 09.95961 -57 06 47.5684 5.01 3.23 1.64 -0.02 -1.44 M3.5III 263 0
12 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1121 0
13 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 340 1
14 HD 139614 pr* 15 40 46.3818973118 -42 29 53.538928508   8.47 8.24     A9VekA5mA5(_lB) 154 0
15 HD 141569 pr* 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 461 0
16 HD 142666 TT* 15 56 40.0222941557 -22 01 40.004849949 9.41 9.37 8.82 8.31 8.01 F0V_sh 209 0
17 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 440 1
18 HD 144432 Ae* 16 06 57.9530266912 -27 43 09.758016578 8.47 8.53 8.19 7.82 7.53 A9/F0V 210 1
19 V* V856 Sco dS* 16 08 34.2868591379 -39 06 18.326059778 7.66 7.41 7.05 6.92   A7 348 0
20 * del Oph PM* 16 14 20.73853 -03 41 39.5612 6.30 4.34 2.75 1.46 0.43 M0.5III 343 0
21 IRAS 16245-2423 TT* 16 27 37.1911764648 -24 30 35.031583716       16.66 14.67 B5-F2 228 0
22 HD 150193 Be* 16 40 17.9242900066 -23 53 45.192676418 9.69 9.32 8.79 8.41   B9.5Ve 288 0
23 * alf TrA * 16 48 39.89508 -69 01 39.7626   3.36 1.92     K2III_Ba1 227 0
24 V* AK Sco Ae* 16 54 44.8497760618 -36 53 18.560813962 9.80 9.63 9.00     F5V 229 1
25 EM* AS 220 Ae* 17 10 08.1238 -27 15 18.801 12.86 12.79 12.22 12.03 10.82 A6Ve+G5Ve 127 0
26 * alf Her ** 17 14 38.85818 +14 23 25.2262   4.51 3.06     M5Ib-II+G5III+F2V: 187 0
27 * c Oph Be* 17 31 24.9541340 -23 57 45.513592 4.75 4.81 4.81 4.74 4.72 A0V 253 0
28 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 757 0
29 * eta Sgr LP? 18 17 37.6350518 -36 45 42.066723 6.37 4.67 3.11 1.55 0.23 M2III 132 1
30 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 318 2
31 V* R CrA Ae* 19 01 53.6850227874 -36 57 08.145519972 12.781 12.651 11.917 11.242 10.412 B5IIIpe 444 1
32 V* T CrA Ae* 19 01 58.7901571143 -36 57 50.329832417     11.67     F0 153 0
33 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 216 0

    Equat.    Gal    SGal    Ecl

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2020.02.18-05:17:10

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