2020A&A...633A.119Z


Query : 2020A&A...633A.119Z

2020A&A...633A.119Z - Astronomy and Astrophysics, volume 633A, 119-119 (2020/1-1)

The widest Hα survey of accreting protoplanets around nearby transition disks.

ZURLO A., CUGNO G., MONTESINOS M., PEREZ S., CANOVAS H., CASASSUS S., CHRISTIAENS V., CIEZA L. and HUELAMO N.

Abstract (from CDS):


Context. The mechanisms of planet formation are still under debate. We know little about how planets form, even if more than 4000 exoplanets have been detected to date. Recent investigations target the cot of newly born planets: the protoplanetary disk. At the first stages of their life, exoplanets still accrete material from the gas-rich disk in which they are embedded. Transitional disks are indeed disks that show peculiarities, such as gaps, spiral arms, and rings, which can be connected to the presence of substellar companions.
Aims. To investigate what is responsible for these features, we selected all the known transitional disks in the solar neighborhood (<200 pc) that are visible from the southern hemisphere. We conducted a survey of 11 transitional disks with the SPHERE instrument at the Very Large Telescope. This is the largest Hα survey that has been conducted so far to look for protoplanets. The observations were performed with the Hα filter of ZIMPOL in order to target protoplanets that are still in the accretion stage. All the selected targets are very young stars, less than 20 Myr, and show low extinction in the visible.
Methods. We reduced the ZIMPOL pupil stabilized data by applying the method of the angular spectral differential imaging (ASDI), which combines both techniques. The datacubes are composed of the Cnt_Hα and the narrow band filter Hα, which are taken simultaneously to permit the suppression of the speckle pattern. The principal component analysis method was employed for the reduction of the data. For each dataset, we derived the 5σ contrast limit and converted it in upper limits on the accretion luminosity.
Results. We do not detect any new accreting substellar companions around the targeted transition disks down to an average contrast of 12 magnitudes at 0.2" from the central star. We have recovered the signal of the accreting M star companion around the star HD 142527. We have detected and resolved, for the first time in visible light, the quadruple system HD 98800. For every other system, we can exclude the presence of massive actively accreting companions, assuming that the accretion is not episodic and that the extinction is negligible. The mean accretion luminosity limit is 10–6L at a separation of 0.2" from the host.

Abstract Copyright: © A. Zurlo et al. 2020

Journal keyword(s): planets and satellites: formation - protoplanetary disks - planet-disk interactions - accretion, accretion disks - techniques: high angular resolution

Simbad objects: 20

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Number of rows : 20
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* UX Tau A TT* 04 30 03.9932216088 +18 13 49.469925504   12.92 11.15     K2Ve 342 0
2 EM* LkCa 15 Or* 04 39 17.7911622816 +22 21 03.390090984   13.01 12.03 11.61   K5:Ve 615 1
3 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 419 0
4 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 497 0
5 HD 98800B SB* 11 22 05.288454 -24 46 39.04974   11.18 9.92     ~ 121 1
6 HD 98800 TT* 11 22 05.28975 -24 46 39.7571   10.20 9.28 9.26 7.386 K5V(e) 353 0
7 HD 99880 PM* 11 29 16.5586666224 -29 21 40.012584120   10.75 9.74     K0/1III 4 0
8 HD 100453 Ae* 11 33 05.5766482920 -54 19 28.547100696   8.09 7.79     A9Ve 243 1
9 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 719 1
10 CPD-68 1894 TT* 13 22 07.5421944624 -69 38 12.219391716   11.38 10.393   9.117 K1Ve 143 0
11 CD-40 8434b Pl 14 08 10.1545137760 -41 23 52.576649494           ~ 126 0
12 CD-40 8434 TT* 14 08 10.1545500744 -41 23 52.573291080   13.42 12.18 11.71 10.506 K7IVe 235 0
13 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 413 1
14 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
15 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 562 1
16 HD 142527b Pl? 15 56 41.8888096574 -42 19 23.245384377           ~ 21 0
17 Haro 1-16 Or* 16 31 33.4634997336 -24 27 37.158728076   14.02 12.80     K3e 205 0
18 V* AK Sco Ae* 16 54 44.8491575376 -36 53 18.566586456 9.80 9.63 9.00     F5V 257 1
19 HD 319139 SB* 18 14 10.4818675368 -32 47 34.516836060   11.47 10.68   9.11 K5+K7 329 0
20 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 388 2

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2022.07.06-08:58:12

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