2023A&A...674A..20D


Query : 2023A&A...674A..20D

2023A&A...674A..20D - Astronomy and Astrophysics, volume 674A, 20 (2023/6-1)

Gaia Data Release 3 Rotational modulation and patterns of colour variation in solar-like variables.

DISTEFANO E., LANZAFAME A.C., BRUGALETTA E., HOLL B., LANZA A.F., MESSINA S., PAGANO I., AUDARD M., JEVARDAT DE FOMBELLE G., LECOEUR-TAIBI I., MOWLAVI N., NIENARTOWICZ K., RIMOLDINI L., EVANS D.W., RIELLO M., GARCIA-LARIO P., GAVRAS P. and EYER L.

Abstract (from CDS):

Context. The Gaia third Data Release (GDR3) presents a catalogue of 474 026 stars (detected by processing a sample of about 30 million late-type stars) with variability induced by magnetic activity. About 430 000 of these stars are newly discovered variables. For each star, the catalogue provides a list of about 70 parameters among which the most important are the stellar rotation period P, the photometric amplitude A of the rotational modulation signal, and the Pearson correlation coefficient r0 between magnitude and colour variation.
Aims. In the present paper we highlight some features of the Gaia photometric time series used to obtain the catalogue and we present the main attributes of the catalogue.
Methods. The Specific Objects Study (SOS) pipeline, developed to characterise magnetically active stars with Gaia data, was described in the paper accompanying the Gaia second rata release (DR2). Here we describe the changes made to the pipeline and a new method developed to analyse Gaia time series and to reveal spurious signals induced by instrumental effects or by the peculiar nature of the investigated stellar source. Such a method is based on the measurement of the per-transit-corrected-excess-factor (c*) for each time-series transit, where c* is a parameter that allows us to check the consistency between G, GBP, and GRP fluxes in a given transit.
Results. The period-amplitude diagram obtained with the DR3 data confirms the DR2 findings that is, the existence of a family of low-amplitude fast rotators never seen by previous surveys. The GDR3 data permit, for the first time, the analysis of patterns in magnitude-colour variation for thousands of magnetically active stars. The measured r0 values are tightly correlated with the star positions in the period-amplitude diagram.
Conclusions. The relationship between the P, A, and r0 parameters inferred for thousands of stars are potentially very useful for improving our understanding of stellar magnetic fields and ameliorating theoretical models, especially in the fast rotation regime. The method developed to reveal the spurious signals can be applied to each of the released Gaia photometric time series and can be exploited by anyone interested in working directly with Gaia time series.

Abstract Copyright: © The Authors 2023

Journal keyword(s): stars: activity - starspots - stars: solar-type - stars: rotation - surveys - techniques: photometric

Simbad objects: 27

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Number of rows : 27
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 2MASS J00343500+4845574 BY* 00 34 35.0129738472 +48 45 57.470507748     14.265     ~ 3 0
2 HAT 87-08179 Ro* 00 49 04.4102419752 +54 27 07.344138708     12.642     ~ 2 0
3 G 272-61B Er* 01 39 01.6377185550 -17 57 01.001240728           M6V 858 0
4 Gaia DR3 508151432071484544 * 01 49 08.8283995392 +60 19 15.901121055           ~ 1 0
5 Gaia DR3 5020821858561059456 * 01 59 21.2367559000 -29 38 08.356835203           ~ 1 0
6 Gaia DR3 5059101630762735360 * 03 06 48.3173932222 -29 42 31.844356590           ~ 1 0
7 2MASS J03073528+4907218 LP* 03 07 35.2885492032 +49 07 21.813110472     13.285     ~ 4 0
8 2MASS J03484771+3504583 PM* 03 48 47.7077741352 +35 04 58.159203024     14.188     ~ 5 0
9 2MASS J05152683-0632010 TT* 05 15 26.8449284640 -06 32 01.022067204           ~ 2 0
10 UCAC4 448-010074 Y*O 05 24 54.6502370304 -00 25 16.743894240       15.38   ~ 7 0
11 V* AB Dor TT* 05 28 44.8712165880 -65 26 55.199147208 8.259 7.856 6.999 6.496 5.993 K0V 1029 0
12 ATO J086.2699+06.2530 BY* 05 45 04.7865555462 +06 15 10.984813451   15.369 14.129 13.747   ~ 4 0
13 Gaia DR3 2925077104599544960 * 06 33 09.3914109995 -22 18 57.440454193           ~ 1 0
14 BD-07 2388 Ro* 08 13 51.0010707504 -07 38 24.864373644   10.18 9.323   8.220 K0 23 0
15 Gaia DR3 5367009382403022592 * 10 37 59.1110360360 -44 36 37.889050999           ~ 1 0
16 V* RS CVn RS* 13 10 36.9077924448 +35 56 05.584994412 8.57 8.51 7.93 7.7   F6IV+G8IV 731 0
17 Gaia DR3 5823916073592266624 * 15 40 10.4272908495 -66 26 37.677490343           ~ 1 0
18 Gaia DR3 6629372460509004928 * 18 01 43.4648225793 -65 54 10.992111373           ~ 1 0
19 V* BY Dra BY* 18 33 55.7720712062 +51 43 08.897780286 10.22 9.23   8.733   K4Ve+K7.5Ve 623 0
20 Gaia DR3 6428392592628180864 * 19 56 35.9203747135 -65 33 08.301978180           ~ 1 0
21 Gaia DR3 1856898294052275840 * 20 28 58.9464074353 +26 51 39.418802494           ~ 1 0
22 ATO J324.0705+36.5280 EB* 21 36 16.9131987084 +36 31 40.969707473   14.437 13.770 13.727   ~ 3 0
23 Gaia DR3 6503897945888972544 PM* 22 46 51.0505438604 -57 34 42.396674241           ~ 1 0
24 Gaia DR3 2624130051834223104 * 22 48 57.2294576511 -04 53 01.550800684           ~ 1 0
25 Gaia DR3 2624130051834565504 * 22 48 57.2551001830 -04 53 01.667620310           ~ 1 0
26 HAT 205-24012 Ro* 22 53 31.8563010960 +37 27 33.043652964     14.582     ~ 2 0
27 NAME Galactic Bulge reg ~ ~           ~ 4360 0

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