2005ApJ...630..958G


Query : 2005ApJ...630..958G

2005ApJ...630..958G - Astrophys. J., 630, 958-975 (2005/September-2)

Coronagraphic imaging of pre-main-sequence stars with the Hubble Space Telescope Space Telescope Imaging Spectrograph. I. The Herbig Ae stars.

GRADY C.A., WOODGATE B.E., BOWERS C.W., GULL T.R., SITKO M.L., CARPENTER W.J., LYNCH D.K., RUSSELL R.W., PERRY R.B., WILLIGER G.M., ROBERGE A., BOURET J.-C. and SAHU M.

Abstract (from CDS):

STIS white-light coronagraphic imaging has been carried out for 14 nearby, lightly reddened Herbig Ae stars, providing data on the environments and disks associated with these stars. No disks are detected in our data when the Herbig Ae star is accompanied by a stellar companion at r≤2''. We find that the optical visibility of protoplanetary disks associated with Herbig Ae stars at r≥50-70 AU from the star is correlated with the strength of the mid-IR PAH features, particularly 6.2 µm. These features, like the FUV fluorescent H2emission, trace the presence of material sufficiently far above the disk midplane that it is directly illuminated by the star's FUV radiation. In contrast, measures of the bulk properties of the disk, including ongoing accretion activity, mass, and the submillimeter slope of the SED, do not correlate with the surface brightness of the optical nebulosity. Modelers have interpreted the appearance of the IR SED and the presence of emission from warm silicate grains at 10 µm as a measure of geometrical shadowing by material in the disk near the dust sublimation radius of 0.5 AU. Geometrical shadowing sufficient to render a disk dark to distances as large as 500 AU from a star would require that the star be optically visible only if viewed essentially pole-on, in disagreement with our program star system inclinations. Rather than invoking shadowing to account for the optically dark disks, the correlation of the STIS detections with PAH emission features suggests a correlation with disk flaring and an anticorrelation with the degree of dust settling toward the midplane. If this correlation continues to lower levels, the STIS data suggest that improvements in coronagraph performance that suppress the residual scattered and diffracted stellar light by an additional factor of ≥10 should render the majority of disks associated with nearby Herbig Ae stars detectable.

Abstract Copyright:

Journal keyword(s): Infrared: Stars - ISM: Herbig-Haro Objects - ISM: Jets and Outflows - Stars: Pre-Main-Sequence

Simbad objects: 28

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Number of rows : 28
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 V* DM Tau Or* 04 33 48.7336763736 +18 10 09.973460280 14.30 14.82 14.00     M2Ve 582 0
2 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 994 2
3 V* SU Aur Or* 04 55 59.3866872552 +30 34 01.499608092   10.33 9.30 9.17   G2IIIne 564 0
4 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 459 0
5 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 419 0
6 V* CQ Tau Ae* 05 35 58.4666264136 +24 44 54.091450572 11.290 10.780 10.000   8.33 F5IVe 283 0
7 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1786 1
8 GD 71 WD* 05 52 27.6198591816 +15 53 13.228887444 11.675 12.783 13.032 13.169 13.337 DA1.5 356 0
9 HD 48099 Be* 06 41 59.2308626256 +06 20 43.532571372 5.38 6.32 6.37 6.30 6.35 O5V((f))z+O9:V 285 0
10 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1745 1
11 HD 95881 Em* 11 01 57.6218887080 -71 30 48.316074624   8.37 8.23     A0 93 0
12 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 719 1
13 V* DX Cha Ae* 12 00 05.0868602544 -78 11 34.565724312   6.81 6.60     A0_sh 321 0
14 HD 109573 PM* 12 36 01.0317461592 -39 52 10.220465388   5.786 5.774 7.25 5.81 A0V 591 1
15 * 61 Vir PM* 13 18 24.3139864471 -18 18 40.297748582 5.710 5.440 4.740     G6.5V 631 1
16 HD 134970 PM* 15 13 50.2575658056 -33 31 04.634979312   9.04 8.56     F5V 12 0
17 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 413 1
18 HD 135344 * 15 15 48.9462675744 -37 08 55.731368400   7.84 7.76     A0V 137 1
19 HD 141653 PM* 15 46 40.0063720128 +62 35 58.403154012   5.240 5.194     A2IV 53 0
20 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 501 0
21 HD 142666 TT* 15 56 40.0221861696 -22 01 40.005872148 9.41 9.37 8.82 8.31 8.01 F0V_sh 239 0
22 HD 144432 Ae* 16 06 57.9533126832 -27 43 09.760564056 8.47 8.53 8.19 7.82 7.53 A9/F0V 228 1
23 V* V856 Sco Ae* 16 08 34.2870044544 -39 06 18.325711332 7.66 7.41 7.05 6.92   A7IIIne_sh 370 0
24 V* V1027 Sco a2* 16 08 34.5616203192 -39 05 34.278268848   6.552 6.629 6.66   A0/3III 184 0
25 NAME Upper Sco-Cen As* 16 15 -24.2           ~ 1232 1
26 HD 150193 Be* 16 40 17.9243127240 -23 53 45.193372692 9.69 9.32 8.79 8.41   B9.5Ve 305 0
27 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 959 0
28 V* AU Mic LM* 20 45 09.5324974119 -31 20 27.237889841   10.05 8.627 9.078 6.593 M1VeBa1 1006 0

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2022.07.06-10:10:17

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