A catalog of blue and red supergiants in M33

Ivanov, G. R.; Freedman, Wendy L.; Madore, Barry F.

doi:10.1086/191840

Cited by 38 publications

(45 citation statements)

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“…The accuracy for the blue star positions is 1B5 (Ivanov et al 1993). None of the red stars in the Ivanov et al (1993) sample match any Chandra source.…”

Section: Other Wavebandsmentioning

confidence: 88%

“…The accuracy for the blue star positions is 1B5 (Ivanov et al 1993). None of the red stars in the Ivanov et al (1993) sample match any Chandra source. Due to the highly clustered nature of the blue supergiants, it is not straightforward to calculate the probability of chance coincidences.…”

Section: Other Wavebandsmentioning

confidence: 88%

“…We cross-correlated our source list with the following catalogs: The XMM-Newton survey of M33 (Pietsch et al 2004), the ROSAT source catalog (Haberl & Pietsch 2001), the catalog of SNRs by Gordon et al (1999), H ii regions from Hodge et al (1999), giant molecular clouds from Engargiola et al (2003), globular clusters from Mochejska et al (1998), star clusters from Chandar et al (1999Chandar et al ( , 2001, blue and red supergiants from Ivanov et al (1993), red supergiants from Massey (1998), WolfRayet stars from Massey & Johnson (1998), UV-bright stars from Massey et al (1996), hot stars from Massey et al (1995), OB associations from Regan & Wilson (1993), planetary nebulae from Magrini et al (2001), H emitters from Calzetti et al (1995), and the DIRECT star catalog from Macri et al (2001).…”

Section: Counterpartsmentioning

confidence: 99%

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The X‐Ray Binary Population in M33. I. Source List and Luminosity Function

Grimm¹,

McDowell²,

Zezas³

et al. 2005

ASTROPHYS J SUPPL S

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In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of $0.2 deg 2 down to a flux limit of 3 ; 10 À16 ergs s À1 cm À2 , which corresponds to a luminosity of $2 ; 10 34 ergs s À1 at a distance of 840 kpc. From the source list we construct the luminosity functions of sources observed in M33. If we take into account background contamination, the luminosity functions are consistent with those of other star-forming galaxies. In addition, the combination of X-ray color analysis and the existence of ''blue'' optical counterparts strongly indicates that the X-ray point-source population in M33 consists of young objects. Above 3 ; 10 35 ergs s À1 there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries.

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“…The accuracy for the blue star positions is 1B5 (Ivanov et al 1993). None of the red stars in the Ivanov et al (1993) sample match any Chandra source.…”

Section: Other Wavebandsmentioning

confidence: 88%

Section: Other Wavebandsmentioning

confidence: 88%

Section: Counterpartsmentioning

confidence: 99%

See 1 more Smart Citation

The X‐Ray Binary Population in M33. I. Source List and Luminosity Function

Grimm¹,

McDowell²,

Zezas³

et al. 2005

ASTROPHYS J SUPPL S

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“…Only one star candidate (#170) could not be associated with the USNO-B1 counterpart, although its HRs and infrared brightness and colour confirm the stellar classification. The source is also listed in the catalogue of blue and red giants in M 33 (Ivanov et al 1993). All of the classified foreground stars and candidates have the X-ray fluxes and hardness ratios in the range expected for this class of objects.…”

Section: Foreground Stars (Fgstar)mentioning

confidence: 99%

An XMM-Newton survey of the Local Group galaxy M 33 – variability of the detected sources

Misanovic

Pietsch

Haberl

et al. 2006

A&A

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We present an analysis of the individual observations of a deep XMM-Newton survey of the Local Group spiral galaxy M 33. We detected a total of 350 sources with fluxes (in the 0.2-4.5 keV energy band) in the range 6.7 × 10 −16 −1.5 × 10 −11 erg s −1 . This comprehensive study considers flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in our catalogue are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. We present improved positions of these sources and the X-ray parameters of each source in each individual observation that covers the source. We then used these parameters to systematically search for flux variability on time scales of hours to months or years. The long-term light-curves were generated for the 61 sources showing a significant variability of the (0.2-4.5) keV flux, by a factor of 1.2 to 144. The detected variability was then used to classify 8 new X-ray binary candidates in M 33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, we also classify or confirm previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, we classify 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M 33. Further 206 objects are classified as "hard", approximately half of which are sources intrinsic to M 33. The relative contribution of the classified XRB and SSS in M 33 is now comparable to M 31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M 33 remains much higher.

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“…Therefore, these values could not be included in the light curves. The catalogue from Ivanov et al (1993) …”

Section: Historical Data Taken From Literaturementioning

confidence: 99%

Var C: Long-term photometric and spectral variability of a luminous blue variable in M 33

Burggraf

Weis

Bomans

et al. 2015

A&A

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Aims. So far the highly unstable phase of luminous blue variables (LBVs) has not been understood well. It is still uncertain why and which massive stars enter this phase. Investigating the variabilities by looking for a possible regular or even (semi-)periodic behaviour could give a hint at the underlying mechanism for these variations and might answer the question of where these variabilities originate. Finding out more about the LBV phase also means understanding massive stars better in general, which have (e.g. by enriching the ISM with heavy elements, providing ionising radiation and kinetic energy) a strong and significant influence on the ISM, hence also on their host galaxy. Methods. Photometric and spectroscopic data were taken for the LBV Var C in M 33 to investigate its recent status. In addition, scanned historic plates, archival data, and data from the literature were gathered to trace Var C's behaviour in the past. Its long-term variability and periodicity was investigated. Results. Our investigation of the variability indicates possible (semi-)periodic behaviour with a period of 42.3 years for Var C. That Var C's light curve covers a time span of more than 100 years means that more than two full periods of the cycle are visible. The critical historic maximum around 1905 is less strong but discernible even with the currently rare historic data. The semi-periodic and secular structure of the light curve is similar to the one of LMC R71. Both light curves hint at a new aspect in the evolution of LBVs.

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A catalog of blue and red supergiants in M33

Cited by 38 publications

References 1 publication

The X‐Ray Binary Population in M33. I. Source List and Luminosity Function

The X‐Ray Binary Population in M33. I. Source List and Luminosity Function

An XMM-Newton survey of the Local Group galaxy M 33 – variability of the detected sources

Var C: Long-term photometric and spectral variability of a luminous blue variable in M 33

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