2013A&A...556A..12P


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.13CET14:28:27

2013A&A...556A..12P - Astronomy and Astrophysics, volume 556A, 12-12 (2013/8-1)

The (non-)variability of magnetic chemically peculiar candidates in the Large Magellanic Cloud.

PAUNZEN E., MIKULASEK Z., POLESKI R., KRTICKA J., NETOPIL M. and ZEJDA M.

Abstract (from CDS):

The galactic magnetic chemically peculiar (mCP) stars of the upper main sequence are well known as periodic spectral and light variables. The observed variability is obviously caused by the uneven distribution of overabundant chemical elements on the surfaces of rigidly rotating stars. The mechanism causing the clustering of some chemical elements into disparate structures on mCP stars has not been fully understood up to now. The observations of light changes of mCP candidates recently revealed in the nearby Large Magellanic Cloud (LMC) should provide us with information about their rotational periods and about the distribution of optically active elements on mCP stars born in other galaxies. We queried for photometry at the Optical Gravitational Lensing Experiment (OGLE)-III survey of published mCP candidates selected because of the presence of the characteristic λ5200Å flux depression. In total, the intersection of both sources resulted in twelve stars. For these objects and two control stars, we searched for a periodic variability. We performed our own and standard periodogram time series analyses of all available data. The final results are, amongst others, the frequency of the maximum peak and the bootstrap probability of its reality. We detected that only two mCP candidates, 190.1 1581 and 190.1 15527, may show some weak rotationally modulated light variations with periods of 1.23 and 0.49 days; however, the 49% and 32% probabilities of their reality are not very satisfying. The variability of the other 10 mCP candidates is too low to be detectable by their V and I OGLE photometry. The relatively low amplitude variability of the studied LMC mCP candidates sample can be explained by the absence of photometric spots of overabundant optically active chemical elements. The unexpected LMC mCPs behaviour is probably caused by different conditions during the star formation in the LMC and the Galaxy.

Abstract Copyright:

Journal keyword(s): stars: chemically peculiar - Magellanic Clouds - stars: variables: general

Simbad objects: 23

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Number of rows : 23

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 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5385 1
2 OGLE LMC136.8 678 Pe* 04 50 05.6794234148 -70 01 29.991947166     17.39     ~ 1 0
3 OGLE LMC136.8 1801 Pe* 04 50 10.90 -70 01 12.8     17.92     ~ 1 0
4 OGLE LMC136.7 861 Pe* 04 50 12.09 -69 59 14.3     16.92     ~ 1 0
5 OGLE LMC136.8 1873 Pe* 04 50 15.50 -70 01 01.1     18.00     ~ 1 0
6 OGLE LMC136.8 2002 Pe* 04 50 24.0293459637 -70 01 49.832568277     18.10     ~ 1 0
7 OGLE LMC136.8 3694 Pe* 04 50 25.90 -70 02 21.7     18.66     ~ 1 0
8 OGLE LMC136.8 3875 Pe* 04 50 33.0644003641 -70 01 00.449644270     18.06     ~ 1 0
9 NGC 1711 Cl* 04 50 37.320 -69 59 01.72   11.22 11.10     ~ 108 0
10 OGLE LMC136.7 16501 Pe* 04 50 46.10 -69 59 16.7     18.24     ~ 1 0
11 OGLE LMC135.3 4273 cC* 04 54 23.0979361992 -69 11 23.973783911     17.770   16.952 ~ 5 0
12 OGLE LMC135.3 30107 Pe* 04 54 57.458 -69 10 41.52     17.02   16.34 ~ 1 0
13 NGC 1866 GlC 05 13 38.920 -65 27 52.75   9.98 9.73     ~ 385 0
14 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14344 1
15 V* V901 Ori Ro* 05 40 56.3704270929 -01 30 25.856714776 5.96 6.82 6.96     B2V 290 2
16 [PMP2006b] 165 Pe* 05 53 01.17 -69 30 12.5     18.36     ~ 2 0
17 NGC 2136 Cl* 05 53 01.800 -69 29 24.24   10.99 10.70     ~ 110 1
18 [PMP2006b] 110 Pe* 05 53 07.85 -69 31 04.0 18.336 18.696 18.738   18.701 ~ 2 0
19 [PMP2006b] 233 Pe* 05 53 13.25 -69 29 36.0 17.351 17.796 17.814   17.915 ~ 2 0
20 [PMP2006b] 91 Pe* 05 53 33.0911271701 -69 31 19.158795668 16.598 17.148 17.193   17.202 ~ 2 0
21 V* CU Vir a2* 14 12 15.8054758 +02 24 33.953395 4.46 4.90 5.02 5.10 5.23 ApSi 342 0
22 V* V771 Her a2* 17 58 52.3061764690 +45 28 34.388554506   6.407 6.481     B9pSiSr 81 0
23 V* EE Dra a2* 18 58 52.6265049377 +69 31 52.643645693   6.353 6.506     B9III 82 1

    Equat.    Gal    SGal    Ecl

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2019.11.13-14:28:27

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