2017A&A...601A.104F


Query : 2017A&A...601A.104F

2017A&A...601A.104F - Astronomy and Astrophysics, volume 601A, 104-104 (2017/5-1)

The effect of ISM absorption on stellar activity measurements and its relevance for exoplanet studies.

FOSSATI L., MARCELJA S.E., STAAB D., CUBILLOS P.E., FRANCE K., HASWELL C.A., INGRASSIA S., JENKINS J.S., KOSKINEN T., LANZA A.F., REDFIELD S., YOUNGBLOOD A. and PELZMANN G.

Abstract (from CDS):

Past ultraviolet and optical observations of stars hosting close-in Jupiter-mass planets have shown that some of these stars present an anomalously low chromospheric activity, significantly below the basal level. For the hot Jupiter planet host WASP-13, observations have shown that the apparent lack of activity is possibly caused by absorption from the intervening interstellar medium (ISM). Inspired by this result, we study the effect of ISM absorption on activity measurements (S and logR'HK indices) for main-sequence late-type stars. To this end, we employ synthetic stellar photospheric spectra combined with varying amounts of chromospheric emission and ISM absorption. We present the effect of ISM absorption on activity measurements by varying several instrumental (spectral resolution), stellar (projected rotational velocity, effective temperature, and chromospheric emission flux), and ISM parameters (relative velocity between stellar and ISM CaII lines, broadening b-parameter, and CaII column density). We find that for relative velocities between the stellar and ISM lines smaller than 30-40km/s and for ISM CaII column densities logNCaII≥12, the ISM absorption has a significant influence on activity measurements. Direct measurements and three dimensional maps of the Galactic ISM absorption indicate that an ISM CaII column density of logNCaII=12 is typically reached by a distance of about 100pc along most sight lines. In particular, for a Sun-like star lying at a distance greater than 100pc, we expect a depression (bias) in the log R'HK value larger than 0.05-0.1dex, about the same size as the typical measurement and calibration uncertainties on this parameter. This work shows that the bias introduced by ISM absorption must always be considered when measuring activity for stars lying beyond 100 pc. We also consider the effect of multiple ISM absorption components. We discuss the relevance of this result for exoplanet studies and revise the latest results on stellar activity versus planet surface gravity correlation. We finally describe methods with which it would be possible to account for ISM absorption in activity measurements and provide a code to roughly estimate the magnitude of the bias. Correcting for the ISM absorption bias may allow one to identify the origin of the anomaly in the activity measured for some planet-hosting stars.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: activity - stars: chromospheres - stars: late-type - ISM: general - planets and satellites: general - planets and satellites: general

Simbad objects: 45

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Number of rows : 45
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 WASP-26 * 00 18 24.7008060816 -15 16 02.275778784   11.62 11.30 10.99 10.46 G0 41 1
2 HAT-P-16 * 00 38 17.5584024024 +42 27 47.216738232   11.38 10.91     F8 54 1
3 CD-50 714 PM* 02 27 06.0975766704 -50 17 04.310799828   10.74 10.14     ~ 31 0
4 WASP-50 * 02 54 45.1341750384 -10 53 53.025224640   12.43 11.44 11.599   G9V 35 1
5 WASP-11 ** 03 09 28.5433589520 +30 40 24.862993356   12.58 11.57 11.42   K3V 74 1
6 WASP-22 * 03 31 16.3267124400 -23 49 10.840600632   12.38 11.99 11.41   G 48 1
7 HD 29587 SB* 04 41 36.3155555021 +42 07 06.424075363 7.940 7.890 7.280 6.74 6.39 G2V 147 1
8 WASP-12 ** 06 30 32.7966092352 +29 40 20.263502460   12.14 11.57     G0V 269 2
9 WASP-12b Pl 06 30 32.7966788910 +29 40 20.266334158           G0 664 1
10 WASP-23 PM* 06 44 30.6133625784 -42 45 42.666796404   13.42 12.52 12.31   ~ 34 1
11 BD+50 1471 PM* 07 48 06.4723053776 +50 13 32.920598923   12.002 11.138 10.669 10.243 G9V 153 1
12 HAT-P-13 * 08 39 31.8072358440 +47 21 07.273799280   11.15 10.42 10.40   G4 123 2
13 BD+02 2056 * 08 44 25.7031511896 +01 51 36.105474888   11.64 10.83     ~ 19 0
14 BD+34 1976 V* 09 20 24.7145388600 +33 52 56.696039796   11.21 10.42     G1V 60 1
15 WASP-19 V* 09 53 40.0765648584 -45 39 33.057187596   13.05 12.31 12.12 11.35 G8V 156 2
16 Ross 905b Pl 11 42 11.0933874353 +26 42 23.658083337           ~ 705 1
17 CD-29 9873 * 12 42 28.4949559632 -30 38 23.529045948   12.36 11.63 11.39 10.78 G8V 49 1
18 WASP-42 PM* 12 51 55.5581398320 -42 04 25.096306584           ~ 23 1
19 HAT-P-3 * 13 44 22.5937349736 +48 01 43.205733624   12.53 11.86     K1V 73 1
20 HAT-P-12 PM* 13 57 33.4668726399 +43 29 36.601508739   12.6 12.84     K5 69 1
21 HAT-P-44 * 14 12 34.5714083256 +47 00 53.044781616   13.2 13.21 12.83 12.31 ~ 18 1
22 WASP-16 * 14 18 43.9225013904 -20 16 31.843626168   12.51 11.29 11.00 10.49 G3V 60 1
23 V* EK Dra BY* 14 39 00.2104038120 +64 17 29.979649860   8.243 7.604     G1.5V 410 0
24 HAT-P-27 * 14 51 04.1870399712 +05 56 50.548526376   13.18 12.19 11.98 11.23 G8 51 1
25 BD+36 2593 * 15 19 57.9203617176 +36 13 46.738078788   11.83 11.12     F 95 1
26 BD+28 2507 V* 16 02 11.8462322592 +28 10 10.420201452   11.88 11.25     G1V 96 1
27 HD 149026 PM* 16 30 29.6185771608 +38 20 50.308980864   8.75 8.14     G0IV 211 1
28 TrES-3 Pl 17 52 07.0185036683 +37 32 46.237002085           ~ 211 2
29 HAT-P-31 * 18 06 09.0498478464 +26 25 35.989962204   12.02 11.67 11.49   ~ 23 2
30 HAT-P-5 * 18 17 37.3126923960 +36 37 17.170401468   12.92 11.95     G1V 58 1
31 NAME V672 Lyr b Pl 19 04 09.8516024106 +36 37 57.445911611           ~ 319 1
32 Kepler-1b Pl 19 07 14.0379171930 +49 18 59.090895318           ~ 302 2
33 WASP-48 * 19 24 38.9614451424 +55 28 23.332107108   12.31 11.65 11.61   ~ 39 1
34 CoRoT-2 * 19 27 06.4944378024 +01 23 01.359897468   13.422 12.568 12.204 11.49 G7V+K9V 229 2
35 HD 189733 BY* 20 00 43.7129433648 +22 42 39.073143456 9.241 8.578 7.648 7.126 6.68 K2V 805 1
36 HD 189733b Pl 20 00 43.7130382888 +22 42 39.071811263           ~ 1263 1
37 WASP-2 V* 20 30 54.1282355304 +06 25 46.341284844   13 11.98     K1.5 124 1
38 HD 358155 ** 21 01 54.480000 -13 25 59.71008   11.75 10.79 11.12   G4+K3 21 1
39 HAT-P-17 PM* 21 38 08.7310010424 +30 29 19.446386748   11.33 10.38 10.24   G0 48 1
40 HD 209458 V* 22 03 10.7727465312 +18 53 03.549393384   8.21 7.63     F9V 1046 1
41 HD 209458b Pl 22 03 10.7729598762 +18 53 03.548248479           ~ 1673 1
42 BD+37 4734B PM* 22 57 46.8442481880 +38 40 30.358351704   10.82 9.87     G0V 150 1
43 WASP-4 PM* 23 34 15.0857248317 -42 03 41.047972591   13.51 12.48 11.9   G7V 149 1
44 WASP-5 V* 23 57 23.7564672192 -41 16 37.743700800   12.808 12.146 12.058 11.44 G4V 104 1
45 NAME Local Bubble ISM ~ ~           ~ 788 0

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2022.07.06-08:44:53

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