J/A+A/589/A113 PMS stars in h Per (Argiroffi+, 2016)
Supersaturation and activity-rotation relation in PMS stars:
the young cluster h Per.
Argiroffi C., Caramazza M., Micela G., Sciortino S., Moraux E., Bouvier J.,
Flaccomio E.
<Astron. Astrophys. 589, A113 (2016)>
=2016A&A...589A.113A 2016A&A...589A.113A (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; ; X-ray sources ; Stars, pre-main sequence
Keywords: stars: activity - stars: coronae - stars: pre-main sequence -
stars: rotation - X-rays: stars
Abstract:
Several studies showed that the magnetic activity of late-type
main-sequence (MS) stars is characterized by different regimes and
that their activity levels are well described by the Ross by number,
Ro, defined as the ratio between the rotational period Prot and the
convective turnover time. Very young pre-main-sequence (PMS) stars
show, similarly to MS stars, intense magnetic activity. However, they
do not show clear activity-rotation trends, and it still debated which
stellar parameters determine their magnetic activity levels.
To bridge the gap between MS and PMS stars, we studied the
activity-rotation relation in the young cluster h Persei, a ∼13Myr old
cluster, that contains both fast and slow rotators. The cluster
members have ended their accretion phase and have developed a
radiative core. It therefore offers us the opportunity of studying the
activity level of intermediate-age PMS stars with different rotational
velocities, excluding any interactions with the circumstellar
environment
We constrained the magnetic activity levels of h Per members by
measuring their X-ray emission from a Chandra observation, while
rotational periods were obtained previously in the framework of the
MONITOR project. By cross-correlating these data, we collected a final
catalog of 414 h Per members with known rotational period, effective
temperature, and mass. In 169 of these, X-ray emission has also been
detected.
Description:
We obtained a deep Chandra/ACIS-I observation of the h Per cluster in
2009. This observation has an exposure time of 189.8ks, it is divided
into three observing segments (Obs ID 09912, 09913, and 12021, PI G.
Micela), and it is centered on RA=02:19:02.20 and DE=+57:07:12.00.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 52 1002 X-ray source detected in the CHANDRA/ACIS-I
observations of h Per
table2.dat 94 795 X-ray source identified as h Per members
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See also:
J/AJ/122/248 : h and chi Per UBVI,Hα photometry (Keller+, 2001)
J/A+A/394/479 : uvbyβ photometry of h and chi Per (Capilla+, 2002)
J/ApJ/576/880 : CCD UBV photometry of h and χ Per (Slesnick+, 2002)
J/PASP/114/233 : h and χ Per memberships (Uribe+, 2002)
J/ApJ/669/L33 : Hα emission sources in h and χ Per (Currie+, 2007)
J/A+A/560/A13 : Stellar rotation in h Per (Moraux+, 2013)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- Seq Sequential number of X source
6 I1 h RAh Right ascension (J2000)
8- 9 I2 min RAm Right ascension (J2000)
11- 15 F5.2 s RAs Right ascension (J2000)
17 A1 --- DE- Declination sign (J2000)
18- 19 I2 deg DEd Declination (J2000)
21- 22 I2 arcmin DEm Declination (J2000)
24- 27 F4.1 arcsec DEs Declination (J2000)
29- 31 F3.1 arcsec e_Pos Positional error
33- 38 F6.1 10-5ct/s CR Count rate in 0.5-8keV band
40- 41 I2 10-5ct/s e_CR rms uncertainty on Count rate
43- 48 F6.1 10-8ph/s/cm2 Flux Flux in 0.5-8keV band
50- 52 I3 10-8ph/s/cm2 e_Flux rms uncertainty on Flux
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- XID ?=- X member sequential number
4 A1 --- n_XID [ab] Multipliicty index on XID
5- 8 I4 --- Seq ?=- Sequential number of X source
10- 12 I3 --- M13 ?=- Moraux et al., 2013, Cat. J/A+A/560/A13
ID, [MAB2013] NNN in Simbad
14- 18 I5 --- C10 ?=- Currie et al., 2010, Cat. J/ApJS/186/191
ID, [CHI2010] h Per MNNNNN in Simbad
20 A1 --- l_logLX Limit flag on logLX
21- 25 F5.2 [10-7W] logLX X-ray luminosity
27- 30 F4.2 [10-7W] E_logLX ? Error on logLX (upper value)
32- 35 F4.2 [10-7W] e_logLX ? Error on logLX (lower value)
37- 42 F6.3 mag Vmag ?=- V magnitude (1)
44- 49 F6.3 mag Imag ?=- I magnitude (1)
51- 55 F5.3 [K] logTeff ?=- Effective temperature
57- 61 F5.3 [K] e_logTeff ? rms uncertainty on logTeff
63- 67 F5.2 [Lsun] logLBol ?=- Bolometric luminosity
69- 72 F4.2 [Lsun] e_logLBol ? rms uncertainty on logLBol
74- 78 F5.2 d Per ?=- Period (2)
80- 83 F4.2 Msun Mass ?=- Mass (2)
85- 89 F5.2 [d] logtau ?=- Age
91- 94 F4.2 [d] e_logtau ?=- rms uncertainty on logtau
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Note (1): From Currie et al., 2010, Cat. J/ApJS/186/191.
Note (2): From Moraux et al., 2013, Cat. J/A+A/560/A13.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 19-Apr-2016