A 2+1+1 quadruple star system containing the most eccentric, low-mass, short-period, eclipsing binary known

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10455943" target="_blank" >RIV/00216208:11320/22:10455943 - isvavai.cz</a>

Result on the web

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=bV1RtmbJtJ" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=bV1RtmbJtJ</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stab3507" target="_blank" >10.1093/mnras/stab3507</a>

Result language

angličtina

Original language name

A 2+1+1 quadruple star system containing the most eccentric, low-mass, short-period, eclipsing binary known

Original language description

We present an analysis of a newly discovered 2+1 + 1 quadruple system with TESS containing an unresolved eclipsing binary (EB) as part of TIC 121088960 and a close neighbour TIC 121088959. The EB consists of two very low-mass M dwarfs in a highly eccentric (e = 0.709) short-period (P = 3.043 58 d) orbit. Given the large pixel size of TESS and the small separation (3.&apos;&apos; 9) between TIC 121088959 and TIC 121088960 we used light centroid analysis of the difference image between in-eclipse and out-of-eclipse data to show that the EB likely resides in TIC 121088960, but contributes only similar to 10 per cent of its light. Radial velocity data were acquired with iSHELL at NASA&apos;s Infrared Facility and the Coude spectrograph at the McDonald 2.7-m telescope. For both images, the measured RVs showed no variation over the 11 d observational baseline, and the RV difference between the two images was 8 +/- 0.3 km s(-1). The similar distances and proper motions of the two images indicate that TIC 121088959 and TIC 121088960 are a gravitationally bound pair. Gaia&apos;s large RUWE and astrometric excess noise parameters for TIC 121088960, further indicate that this image is the likely host of the unresolved EB and is itself a triple star. We carried out an SED analysis and calculated stellar masses for the four stars, all of which are in the M dwarf regime: 0.19 M-circle dot and 0.14 M-circle dot for the EB stars and 0.43 M-circle dot and 0.39 M-circle dot for the brighter visible stars, respectively. Lastly, numerical simulations show that the orbital period of the inner triple is likely the range 1-50 yr.

Czech name

—

Czech description

—

Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

—

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2022

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Volume of the periodical

510

Issue of the periodical within the volume

2

Country of publishing house

GB - UNITED KINGDOM

Number of pages

16

Pages from-to

2448-2463

UT code for WoS article

000744576900053

EID of the result in the Scopus database

2-s2.0-85126392768