2017A&A...598A..28S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST21:34:26

2017A&A...598A..28S - Astronomy and Astrophysics, volume 598A, 28-28 (2017/2-1)

HADES RV Programme with HARPS-N at TNG. IV. Time resolved analysis of the Ca II H&K and Hα chromospheric emission of low-activity early-type M dwarfs.

SCANDARIATO G., MALDONADO J., AFFER L., BIAZZO K., LETO G., STELZER B., ZANMAR SANCHEZ R., CLAUDI R., COSENTINO R., DAMASSO M., DESIDERA S., GONZALEZ-ALVAREZ E., GONZALEZ HERNANDEZ J.I., GRATTON R., LANZA A.F., MAGGIO A., MESSINA S., MICELA G., PAGANO I., PERGER M., PIOTTO G., REBOLO R., RIBAS I., ROSICH A., SOZZETTI A. and SUAREZ MASCARENO A.

Abstract (from CDS):

Context. M dwarfs are prime targets for current and future planet search programs, particularly those focused on the detection and characterization of rocky planets in the habitable zone. In this context, understanding their magnetic activity is important for two main reasons: it affects our ability to detect small planets and it plays a key role in the characterization of the stellar environment.
Aims. We analyze observations of the CaII H&K and Hα lines as diagnostics of chromospheric activity for low-activity early-type M dwarfs.
Methods. We analyze the time series of spectra of 71 early-type M dwarfs collected in the framework of the HADES project for planet search purposes. The HARPS-N spectra simultaneously provide the CaII H&K doublet and the Hα line. We develop a reduction scheme able to correct the HARPS-N spectra for instrumental and atmospheric effects, and also to provide flux-calibrated spectra in units of flux at the stellar surface. The CaII H&K and Hα fluxes are then compared with each other, and their time variability is analyzed.
Results. We find that the CaII H and K flux excesses are strongly correlated with each other, while the Hα flux excess is generally less correlated with the CaII H&K doublet. We also find that Hα emission does not increase monotonically with the CaII H&K line flux, showing some absorption before being filled in by chromospheric emission when CaII H&K activity increases. Analyzing the time variability of the emission fluxes, we derive a tentative estimate of the rotation period (on the order of a few tens of days) for some of the program stars, and the typical lifetime of chromospheric active regions (on the order of a few stellar rotations).
Conclusions. Our results are in good agreement with similar previous studies. In particular, we find evidence that the chromospheres of early-type M dwarfs could be characterized by different filament coverage, affecting the formation mechanism of the Hα line. We also show that chromospheric structure is likely related to spectral type.

Abstract Copyright: © ESO, 2017

Journal keyword(s): techniques: spectroscopic - stars: late-type - stars: low-mass - stars: activity

Simbad objects: 72

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Number of rows : 72

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 BD+44 4548 PM* 00 05 10.8891772602 +45 47 11.639549811   11.45   9.2   M2Ve 132 0
2 G 242-48 Fl* 00 13 38.7121759050 +80 39 56.841311586       10.681   M1.5V 51 0
3 GJ 16 * 00 18 16.5899263489 +10 12 10.038660333 13.572 12.39 10.864 9.869 8.738 M1V 46 0
4 V* GX And Er* 00 18 22.8849667932 +44 01 22.637271919   10.120   7.3   M2V 448 0
5 GJ 21 PM* 00 26 52.7020266762 +70 08 32.718092385   11.8   10.075   M1.0Ve 40 0
6 Wolf 1056 PM* 00 38 59.0436387491 +30 36 58.387293197   12.60   10.6   M2.5V 71 0
7 Wolf 44 PM* 01 01 20.0490626127 +61 21 56.681939701   12.26 10.87     M2.0Ve 64 1
8 BD+61 195 PM* 01 02 38.8679928575 +62 20 42.172837073   11.439   8.7   M1.5V 191 0
9 G 33-36 PM* 01 06 41.5115096766 +15 16 22.089897047 14.124 12.913 11.403 10.415 9.232 M0V 38 0
10 Wolf 59 PM* 01 16 10.1311678064 +60 09 12.828596681       10.801   M0.5Ve 19 0
11 G 3-14 PM* 01 43 20.1788090313 +04 19 17.962195740 13.64 12.45 10.915 9.879 8.614 M2V 116 0
12 G 244-37 PM* 01 51 51.1324314626 +64 26 05.922097987       11.036   M2.5Ve 34 0
13 G 244-47 PM* 02 01 35.3406953145 +63 46 11.995703079       10.630   M2.5Ve 45 0
14 G 36-38 PM* 02 52 25.0253120212 +26 58 29.928150679   12.11 11.048 10.646   M2V 40 0
15 Ross 364 PM* 02 56 34.4247155101 +55 26 14.099190043       9.6   M1.0Ve 56 0
16 Ross 365 PM* 02 56 35.1558957639 +55 26 29.610494191   13.0   10.9   M2.5Ve 42 0
17 StKM 1-347 PM* 03 12 12.6309933986 +29 51 32.416368856   12.20 11.056 10.62   K7.5Ve 11 0
18 LP 198-637 ** 03 20 45.215160 +39 43 01.47432   12.74 11.31 10.82   M1.5Ve 16 0
19 HIP 17248 PM* 03 41 37.2770784530 +55 13 06.829383692 15.431     10.794   M0.0V 37 0
20 MCC 428 PM* 03 43 45.2472698195 +16 40 02.169395779 13.476 12.265 10.763 9.78 8.681 M0V 72 0
21 Ross 23 PM* 03 56 47.3993665960 +53 33 36.798790387   12.29   10.572   M1.5Ve 42 0
22 HD 281621 PM* 04 08 37.3989601715 +33 38 13.332607300   11.69 10.213 9.734 8.19 K7V 64 0
23 G 191-15 Ro* 04 58 45.9906833818 +50 56 37.765807469   12.39   10.1   M1.0Ve 48 0
24 BD+52 911 PM* 05 03 23.9014100324 +53 07 42.487841299   11.789 10.059 9.08 8.11 M0.5Ve 82 0
25 G 191-45 PM* 05 34 08.6634642422 +51 12 56.366607272   12.35 11.069 10.593   M1.0Ve 32 0
26 StKM 1-587 Ro* 06 14 42.4166712254 +47 27 34.600460523   12.86 11.428 11.012   M0.5Ve 12 0
27 LF 8 +13 265 PM* 06 19 29.4972346270 +13 57 02.967216243   12.03 10.708 10.171   M0.5Ve 13 0
28 G 107-65 PM* 07 23 14.8951251540 +46 05 14.685421330       10.059   M1V 63 0
29 StKM 1-650 PM* 07 31 36.1454923396 +62 01 11.524336140   13.36   11.436   M0.5Ve 13 0
30 G 234-57 PM* 09 13 23.849448 +68 52 30.70416   12.77 11.17 10.76   M2.5V 25 0
31 G 55-35 PM* 10 39 40.5642980607 -06 55 25.501668469 13.939 12.79 11.281 10.244 8.961 M2.5 61 0
32 Ross 104 PM* 11 00 04.2569699829 +22 49 58.646653116 12.826 11.584 10.020 8.952 7.646 M4V 144 0
33 BD+44 2051 PM* 11 05 28.57798 +43 31 36.3914 11.440 10.270   7.9   M1.0Ve 267 0
34 HD 97101B PM* 11 11 02.5375659927 +30 26 41.317154374   12.39 9.983 8.99 7.83 M2V 100 0
35 GJ 3649 * 11 12 38.9716051201 +18 56 05.435176426   12.19 10.85     M1 30 0
36 MCC 135 LM* 11 51 07.3365548593 +35 16 19.248830169   11.30 9.802 9.420 7.64 M1.5V 142 0
37 BD+29 2279 PM* 12 19 24.0910326997 +28 22 56.540696752   10.705   9.8   M0.5Ve 86 0
38 Wolf 427 PM* 12 35 00.7054724850 +09 49 42.567052394 13.884 12.85 11.405 10.413 9.171 M1V 60 1
39 Ross 1007 PM* 13 19 40.1257231213 +33 20 47.508531100   12.16   10.179   M2V 97 0
40 BD+46 1889 ** 13 39 24.1024718496 +46 11 11.364403506       9.800   M1.0V 80 0
41 GJ 3822 PM* 14 02 19.6250412883 +13 41 22.687171479 13.34 12.098 10.636 9.691 8.678 M1V 49 0
42 BD+24 2733 PM* 14 25 43.4748768148 +23 37 01.493445118 12.398 11.169 9.720 8.811 7.877 M3V 91 0
43 BD+16 2658 PM* 14 29 29.6973349522 +15 31 57.498714295 13.385 12.176 10.676 9.674 8.467 M2/3V 105 0
44 BD-07 4156 PM* 15 59 53.3815624277 -08 15 11.541690269 13.197 11.999 10.487 9.497 8.365 M1V 55 0
45 GJ 3942 PM* 16 09 03.1411378130 +52 56 37.958424161       9.706   M0.5Ve 46 0
46 G 202-48 PM* 16 25 24.6233091302 +54 18 14.765751243       9.664   M1.5V 153 0
47 BD+19 3268 ** 17 15 50.1150 +19 00 00.072   11.80 10.370 9.864   M0.5Ve 28 0
48 BD+11 3149 PM* 17 16 00.6367305760 +11 03 27.613687917 13.521 12.338 10.828 9.858 8.767 M1V 49 0
49 G 139-27 PM* 17 16 40.9809926333 +08 03 30.204061380 14.301 13.087 11.529 10.48 9.219 M2.5Ve 51 0
50 G 181-39 PM* 17 19 52.7126409684 +41 42 49.698739005   11.423   10.4   M2V 73 0
51 G 226-66 PM* 17 35 34.4785948351 +61 40 53.626580217   11.40 9.98 9.52 8.01 M1V 105 0
52 BD+18 3421 PM* 17 37 53.3467427850 +18 35 30.160739363 12.315 11.109 9.577 8.599 7.525 M1.5Ve 160 0
53 BD+43 2796 PM* 17 43 55.9631098729 +43 22 43.000698258   12.05   10.066   M2V 110 0
54 BD+46 2361 * 17 45 33.5265604481 +46 51 19.303906570   12.09 10.718 10.194   M1V 53 0
55 HD 336196 PM* 18 25 04.7943323101 +24 38 04.480561918 13.477 12.26 10.767 9.847 8.894 M0V 34 1
56 BD+45 2743 PM* 18 35 18.3905783079 +45 44 38.536570500   11.26 9.830 9.400 8 M0.5V 103 0
57 HD 229793 PM* 18 51 51.1836152719 +16 34 59.814863531 12.787 11.585 10.104 9.174 8.23 M0V 71 0
58 HD 176029 PM* 18 58 00.1362110113 +05 54 29.238610798 11.888 10.673 9.217 8.286 7.31 M1.0Ve 122 0
59 BD+07 3922 PM* 18 59 38.6064621031 +07 59 14.116372831       10.368   M0.5Ve 29 0
60 Ross 754 PM* 20 13 51.8072664687 +13 23 19.714152997       10.827   K6V 26 0
61 G 262-15 PM* 20 30 32.0455058633 +65 26 58.410103877   12.00   10.124   M3V 129 0
62 BPM 96441 PM* 21 12 55.4530377873 +31 07 54.300629941   13.3 11.9 11.069   K7/M0V 10 0
63 PM J21179+3404 ** 21 17 59.0727 +34 04 30.151   12.94 11.52 11.07   M0.0Ve 12 0
64 StKM 1-1877 PM* 21 18 33.7570277672 +30 14 34.620165746   13.24 11.69 11.154   M1.5V 21 0
65 V* V2160 Cyg Ro* 21 27 32.9566593386 +34 01 28.640453919       10.668   M1.5Ve 30 0
66 BD+43 4035 PM* 21 44 53.9918673368 +44 17 08.905809769   12.61 11.342 10.919 9.25 M2+V 33 0
67 G 214-14 PM* 22 11 16.9512260570 +41 00 54.831180528       10.559   M0.0Ve 29 0
68 UCAC4 637-120205 PM* 22 35 35.0329193755 +37 12 13.115068417     11.771 11.316   M0.0Ve 9 0
69 BD+18 5029 PM* 22 41 35.0151717013 +18 49 27.335539902       10.272   M0V 31 0
70 GJ 4306 PM* 22 55 59.8455810494 +17 48 39.799225271   11.76 10.558 10.063   M1.0Ve 22 0
71 BD+57 2735 PM* 23 24 30.5145080333 +57 51 15.516771965   11.56   9.586   M1.5Ve 93 0
72 V* BR Psc BY* 23 49 12.5251391270 +02 24 04.403044891 11.532 10.427 8.993 8.029 6.946 M1VFe-1 282 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-21:34:26

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