2019A&A...622A..93B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.12CEST14:50:03

2019A&A...622A..93B - Astronomy and Astrophysics, volume 622A, 93-93 (2019/2-1)

CI Camelopardalis: The first sgB[e]-high mass X-ray binary twenty years on: A supernova imposter in our own Galaxy?

BARTLETT E.S., CLARK J.S. and NEGUERUELA I.

Abstract (from CDS):


Context. The Galactic supergiant B[e] star CI Camelopardalis (CI Cam) was the first sgB[e] star detected during an X-ray outburst. The star brightened to ∼2Crab in the X-ray regime (∼5x10–8ergs/cm2/s in the 2-25keV range) within hours before decaying to a quiescent level in less than two weeks, clearly indicative of binarity. Since the outburst of CI Cam, several sgB[e] stars have been identified as X-ray overluminous for a single star (i.e. LX>10–7Lbol). This small population has recently expanded to include two ultra luminous X-ray sources (ULX), Holmberg II X-1 and NGC 300 ULX-1/supernova imposter SN2010da.
Aims. Since the discovery of X-ray emission from CI Cam, there have been many developments in the field of massive binary evolution. In light of the recent inclusion of two ULXs in the population of X-ray bright sgB[e] stars, we revisit CI Cam to investigate its behaviour over several timescales and shed further light on the nature of the compact object in the system, its X-ray outburst in 1998 and the binary system parameters.
Methods. We analysed archival XMM-Newton EPIC-pn spectra and light curves along with new data from Swift and NuSTAR. We also present high-resolution (R∼85000) Mercator/HERMES optical spectra, including a spectrum taken 1.02 days after our NuSTAR observation.
Results. Despite being in quiescence, CI Cam is highly X-ray variable on timescales of days, both in terms of total integrated flux and spectral shape. We interpret these variations by invoking the presence of an accreting compact companion immersed in a dense, highly structured, aspherical circumstellar envelope. The differences in the accretion flux and circumstellar extinction represent either changes in this environment, triggered by variable mass loss from the star, or the local conditions to the accretor due to its orbital motion. We find no evidence for pulsations in the X-ray light curve.
Conclusions. CI Cam has many similarities with SN2010da across mid-IR, optical and X-ray wavelengths suggesting that, subject to distance determination for CI Cam, if CI Cam was located in an external galaxy its 1998 outburst would have led to a classification as a supernova imposter.

Abstract Copyright: © ESO 2019

Journal keyword(s): stars: emission-line, Be - pulsars: individual: CI Camelopardalis - stars: massive - binaries: general - X-rays: binaries

Simbad objects: 22

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Number of rows : 22

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 IC 10 X-1 HXB 00 20 29.09 +59 16 51.9           ~ 148 0
2 LHA 115-S 6 s*b 00 46 55.0295095056 -73 08 34.139503944 12.14 13.02 12.91   12.52 B0/0.5[e] 77 1
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9446 1
4 LHA 115-S 18 Em* 00 54 09.5415603586 -72 41 43.291670748 12.94 13.48 13.82   12.55 B[e] 76 0
5 NAME NGC 300 2010da s*b 00 55 04.86 -37 41 43.7           LBV 96 0
6 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5669 1
7 V* CI Cam HXB 04 19 42.1353986687 +55 59 57.708146070 12.13 12.41 11.77 10.79 9.99 B0/2I[e] 224 0
8 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4485 2
9 HD 38489 s*b 05 40 13.3208554964 -69 22 46.485104413 11.236 12.295 11.93 11.79 10.891 B[e] 81 1
10 [SST2011] J081929.00+704219.3 ULX 08 19 28.99 +70 42 19.4           ~ 157 2
11 SN 2006jc SN* 09 17 20.78 +41 54 32.7     13.8     SNIbn 264 1
12 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2201 0
13 SN 2000ch SN* 10 52 41.40 +36 40 09.5     17.4     SNIIn? 84 2
14 HD 94878 bL* 10 55 58.9150038252 -60 23 33.434805592 8.67 9.37 8.70 8.07   B0/2eq 139 0
15 IGR J16318-4848 HXB 16 31 48.3102815892 -48 49 00.664215918           ~ 157 0
16 Cl* Westerlund 1 W 9 WR* 16 47 04.1422943113 -45 50 31.307461802   21.8 17.47 14.47 11.74 Be 46 0
17 SN 2010mc SN* 17 21 30.68 +48 07 47.4           SNIIn 61 1
18 2MASS J18211975-1318388 HXB 18 21 19.7677353711 -13 18 39.091923453           B0V-O9I 29 0
19 [KRL2007b] 332 HXB 18 41 00.43 -05 35 46.5           B1Ib 115 1
20 SS 433 HXB 19 11 49.5645897701 +04 58 57.824087535   16.3 13.0     A7Ib: 1928 3
21 SN 2009da SN* 21 42 07.20 -06 46 25.6           SNIa 5 1
22 SN 2009ip s*b 22 23 08.26 -28 56 52.4           LBV 266 0

    Equat.    Gal    SGal    Ecl

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2020.07.12-14:50:03

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