2017A&A...598A..27M


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.06CET01:04:22

2017A&A...598A..27M - Astronomy and Astrophysics, volume 598A, 27-27 (2017/2-1)

HADES RV Programme with HARPS-N at TNG. III. Flux-flux and activity-rotation relationships of early-M dwarfs.

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

Abstract (from CDS):

Context. Understanding stellar activity in M dwarfs is crucial for the physics of stellar atmospheres and for ongoing radial velocity exoplanet programmes. Despite the increasing interest in M dwarfs, our knowledge of the chromospheres of these stars is far from being complete.
Aims. We test whether the relations between activity, rotation, and stellar parameters and flux-flux relationships previously investigated for main-sequence FGK stars and for pre-main-sequence M stars also hold for early-M dwarfs on the main-sequence. Although several attempts have been made so far, here we analyse a large sample of stars undergoing relatively low activity.
Methods. We analyse in a homogeneous and coherent way a well-defined sample of 71 late-K/early-M dwarfs that are currently being observed in the framework of the HArps-N red Dwarf Exoplanet Survey (HADES). Rotational velocities are derived using the cross-correlation technique, while emission flux excesses in the CaII H & K and Balmer lines from Hα up to Hε are obtained by using the spectral subtraction technique. The relationships between the emission excesses and the stellar parameters (projected rotational velocity, effective temperature, kinematics, and age) are studied. Relations between pairs of fluxes of different chromospheric lines (flux-flux relationships) are also studied and compared with the literature results for other samples of stars.
Results. We find that the strength of the chromospheric emission in the CaII H & K and Balmer lines is roughly constant for stars in the M0-M3 spectral range. Although our sample is likely to be biased towards inactive stars, our data suggest that a moderate but significant correlation between activity and rotation might be present, as well as a hint of kinematically selected young stars showing higher levels of emission in the calcium line and in most of the Balmer lines. We find our sample of M dwarfs to be complementary in terms of chromospheric and X-ray fluxes with those of the literature, extending the analysis of the flux-flux relationships to the very low flux domain.
Conclusions. Our results agree with previous works suggesting that the activity-rotation-age relationship known to hold for solar-type stars also applies to early-M dwarfs. We also confirm previous findings that the field stars which deviate from the bulk of the empirical flux-flux relationships show evidence of youth.

Abstract Copyright: © ESO, 2017

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

Simbad objects: 77

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Number of rows : 77

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 BD+44 4548 PM* 00 05 10.8891772602 +45 47 11.639549811   11.45   9.2   M2Ve 142 0
2 G 242-48 Er* 00 13 38.7121759050 +80 39 56.841311586       10.681   M1.5V 54 0
3 GJ 16 * 00 18 16.5899263489 +10 12 10.038660333 13.572 12.39 10.864 9.869 8.738 M1V 48 0
4 V* GX And Er* 00 18 22.8849667932 +44 01 22.637271919   10.120   7.3   M2V 464 0
5 GJ 21 PM* 00 26 52.7020266762 +70 08 32.718092385   11.8   10.075   M1.0Ve 43 0
6 Wolf 1056 PM* 00 38 59.0436387491 +30 36 58.387293197   12.60   10.6   M2.5V 80 0
7 Wolf 44 PM* 01 01 20.0490626127 +61 21 56.681939701   12.26 10.87     M2.0Ve 73 1
8 BD+61 195 PM* 01 02 38.8679928575 +62 20 42.172837073   11.439   8.7   M1.5V 206 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 40 0
10 Wolf 59 PM* 01 16 10.1311678064 +60 09 12.828596681       10.801   M0.5Ve 21 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 126 0
12 G 244-37 PM* 01 51 51.1324314626 +64 26 05.922097987       11.036   M2.5Ve 42 0
13 G 244-47 PM* 02 01 35.3406953145 +63 46 11.995703079       10.630   M2.5Ve 54 0
14 G 36-38 PM* 02 52 25.0253120212 +26 58 29.928150679   12.11 11.048 10.646   M2V 42 0
15 Ross 364 PM* 02 56 34.4247155101 +55 26 14.099190043       9.6   M1.0Ve 66 0
16 Ross 365 PM* 02 56 35.1558957639 +55 26 29.610494191   13.0   10.9   M2.5Ve 44 0
17 StKM 1-347 PM* 03 12 12.6309933986 +29 51 32.416368856   12.20 11.056 10.62   K7.5Ve 12 0
18 LP 198-637 ** 03 20 45.215160 +39 43 01.47432   12.74 11.31 10.82   M1.5Ve 18 0
19 HIP 17248 PM* 03 41 37.2770784530 +55 13 06.829383692 15.431     10.794   M0.0V 39 0
20 MCC 428 PM* 03 43 45.2472698195 +16 40 02.169395779 13.476 12.265 10.763 9.78 8.681 M0V 75 0
21 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 3064 0
22 Ross 23 PM* 03 56 47.3993665960 +53 33 36.798790387   12.29   10.572   M1.5Ve 44 0
23 HD 281621 ** 04 08 37.3989601715 +33 38 13.332607300   11.872 10.192 9.734 8.19 K7V 66 0
24 G 191-15 Ro* 04 58 45.9906833818 +50 56 37.765807469   12.39   10.1   M1.0Ve 50 0
25 BD+52 911 PM* 05 03 23.9014100324 +53 07 42.487841299   11.789 10.059 9.08 8.11 M0.5Ve 85 0
26 G 191-45 PM* 05 34 08.6634642422 +51 12 56.366607272   12.35 11.069 10.593   M1.0Ve 34 0
27 NAME Columba Association As* 06 14.0 -40 03           ~ 217 0
28 StKM 1-587 Ro* 06 14 42.4166712254 +47 27 34.600460523   12.86 11.428 11.012   M0.5Ve 13 0
29 LF 8 +13 265 PM* 06 19 29.4972346270 +13 57 02.967216243   12.03 10.708 10.171   M0.5Ve 14 0
30 G 107-65 PM* 07 23 14.8951251540 +46 05 14.685421330       10.059   M1V 65 0
31 StKM 1-650 PM* 07 31 36.1454923396 +62 01 11.524336140   13.36   11.436   M0.5Ve 14 0
32 Ass Vel OB 2 As* 08 09 22.478 -47 21 03.46           ~ 223 0
33 G 234-57 PM* 09 13 23.849448 +68 52 30.70416   12.77 11.17 10.76   M2.5V 32 0
34 G 55-35 PM* 10 39 40.5642980607 -06 55 25.501668469 13.939 12.79 11.281 10.244 8.961 dM2.5 68 0
35 Ross 104 PM* 11 00 04.2569699829 +22 49 58.646653116 12.826 11.584 10.020 8.952 7.646 M4V 152 0
36 BD+44 2051 PM* 11 05 28.57798 +43 31 36.3914 11.440 10.270   7.9   M1.0Ve 275 0
37 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1011 1
38 HD 97101B PM* 11 11 02.5375659927 +30 26 41.317154374   12.39 9.983 8.99 7.83 M2V 105 0
39 GJ 3649 * 11 12 38.9716051201 +18 56 05.435176426   12.19 10.85     dM1.5 36 0
40 MCC 135 LM* 11 51 07.3365548593 +35 16 19.248830169   11.30 9.802 9.420 7.64 M1.5V 150 0
41 BD+29 2279 PM* 12 19 24.0910326997 +28 22 56.540696752   10.705   9.8   M0.5Ve 89 0
42 Wolf 427 PM* 12 35 00.7054724849 +09 49 42.567052394 13.884 12.85 11.405 10.413 9.171 M1V 66 1
43 Ross 1007 PM* 13 19 40.1257231213 +33 20 47.508531100   12.16   10.179   M2V 105 0
44 BD+46 1889 ** 13 39 24.1024718496 +46 11 11.364403506       9.800   M1.0V 83 0
45 * eta UMa PM* 13 47 32.43776 +49 18 47.7602 0.99 1.67 1.86 1.98 2.16 B3V 583 0
46 GJ 3822 PM* 14 02 19.6250412883 +13 41 22.687171479 13.34 12.098 10.636 9.691 8.678 M1V 51 0
47 BD+24 2733 PM* 14 25 43.4748768148 +23 37 01.493445118 12.398 11.169 9.720 8.811 7.877 M3V 98 0
48 BD+16 2658 PM* 14 29 29.6973349522 +15 31 57.498714295 13.385 12.176 10.676 9.674 8.467 M2/3V 112 0
49 BD-07 4156 PM* 15 59 53.3815624277 -08 15 11.541690269 13.197 11.999 10.487 9.497 8.365 M1V 62 0
50 GJ 3942 PM* 16 09 03.1411378130 +52 56 37.958424161       9.706   M0.5Ve 49 0
51 G 202-48 PM* 16 25 24.6233091302 +54 18 14.765751243   11.78 10.07 9.66   M1.5V 166 0
52 BD+19 3268 ** 17 15 50.1150 +19 00 00.072   11.80 10.370 9.864   M0.5Ve 31 0
53 BD+11 3149 PM* 17 16 00.6367305760 +11 03 27.613687917 13.521 12.338 10.828 9.858 8.767 M1V 51 0
54 G 139-27 PM* 17 16 40.9809926333 +08 03 30.204061380 14.301 13.087 11.529 10.48 9.219 M2.5Ve 59 0
55 G 181-39 PM* 17 19 52.7126409684 +41 42 49.698739005   11.423   10.4   M2V 80 0
56 G 226-66 PM* 17 35 34.4785948351 +61 40 53.626580217   11.40 9.98 9.52 8.01 M1V 115 0
57 BD+18 3421 PM* 17 37 53.3467427850 +18 35 30.160739363 12.315 11.109 9.577 8.599 7.525 M1.5Ve 172 0
58 BD+46 2361 * 17 45 33.5265604481 +46 51 19.303906570   12.09 10.718 10.194   M1V 55 0
59 HD 336196 PM* 18 25 04.7943323101 +24 38 04.480561918 13.477 12.26 10.767 9.847 8.894 M0V 36 1
60 BD+45 2743 PM* 18 35 18.3905783079 +45 44 38.536570500   11.26 9.830 9.400 8 M0.5V 111 0
61 HD 229793 PM* 18 51 51.1836152719 +16 34 59.814863531 12.787 11.585 10.104 9.174 8.23 M0V 74 0
62 HD 176029 PM* 18 58 00.1362110113 +05 54 29.238610798 11.888 10.673 9.217 8.286 7.31 M1.0Ve 129 0
63 BD+07 3922 PM* 18 59 38.6064621031 +07 59 14.116372831       10.368   M0.5Ve 31 0
64 Ross 754 PM* 20 13 51.8072664687 +13 23 19.714152997       10.827   K6V 28 0
65 G 262-15 PM* 20 30 32.0455058633 +65 26 58.410103877   12.00   10.124   M3V 137 0
66 BPM 96441 PM* 21 12 55.4530377873 +31 07 54.300629941   13.3 11.9 11.069   K7/M0V 10 0
67 PM J21179+3404 ** 21 17 59.0727 +34 04 30.151   12.94 11.52 11.07   M0.0Ve 13 0
68 StKM 1-1877 PM* 21 18 33.7570277672 +30 14 34.620165746   13.24 11.69 11.154   M1.5V 23 0
69 V* V2160 Cyg Ro* 21 27 32.9566593386 +34 01 28.640453919       10.668   M1.5Ve 32 0
70 G 215-12 PM* 21 44 53.9918673368 +44 17 08.905809769   12.61 11.342 10.919 9.25 M2+V 34 0
71 G 214-14 PM* 22 11 16.9512260570 +41 00 54.831180528       10.559   M0.0Ve 31 0
72 UCAC4 637-120205 PM* 22 35 35.0329193755 +37 12 13.115068417     11.771 11.316   M0.0Ve 9 0
73 BD+18 5029 PM* 22 41 35.0151717012 +18 49 27.335539902       10.272   M0V 34 0
74 GJ 4306 PM* 22 55 59.8455810494 +17 48 39.799225271   11.76 10.558 10.063   M1.0Ve 28 0
75 BD+57 2735 PM* 23 24 30.5145080333 +57 51 15.516771965   11.56   9.586   M1.5Ve 101 0
76 V* BR Psc BY* 23 49 12.5251391270 +02 24 04.403044891 11.532 10.427 8.993 8.029 6.946 dM1 290 0
77 NAME Pleiades Moving Group MGr ~ ~           ~ 243 1

    Equat.    Gal    SGal    Ecl

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2021.03.06-01:04:22

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