Peter Weiss's Documentary Theater

Haberl, Franz P.

doi:10.2307/40123536

Cited by 19 publications

(50 citation statements)

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“…Source 1745 [source 84 in Haberl & Sturm (2016)] lies in the overlapping region between hard and intermediate state accreting black holes and accreting pulsars on the diagnostic diagrams. Thus far source 1745 has been identified as a Be-XRB (Meyssonnier & Azzopardi 1993;Haberl & Sasaki 2000;Antoniou et al 2009;Haberl & Sturm 2016) with a clear emission-line star as its optical counterpart. Its X-ray spectrum is typical of an X-ray binary with Γ < 1.3 (Haberl & Sturm 2016).…”

Section: Source 1745 -Low Luminosity Be-xrbmentioning

confidence: 99%

Neutron Stars and Black Holes in the Small Magellanic Cloud: The SMC NuSTAR Legacy Survey

Lazzarini

Williams

Hornschemeier

et al. 2019

ApJ

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We present a source catalog from the first deep hard X-ray (E > 10 keV) survey of the Small Magellanic Cloud (SMC), the NuSTAR Legacy Survey of the SMC. We observed three fields, for a total exposure time of 1 Ms, along the bar of this nearby star-forming galaxy. Fields were chosen for their young stellar and accreting binary populations. We detected 10 sources above a 3σ significance level (4-25 keV) and obtained upper limits on an additional 40 sources. We reached a 3σ limiting luminosity in the 4-25 keV band of ∼ 10 35 erg s −1 , allowing us to probe fainter X-ray binary (XRB) populations than has been possible with other extragalactic NuSTAR surveys. We used hard X-ray colors and luminosities to constrain the compact-object type, exploiting the spectral differences between accreting black holes and neutron stars at E > 10 keV. Several of our sources demonstrate variability consistent with previously observed behavior. We confirmed pulsations for seven pulsars in our 3σ sample. We present the first detection of pulsations from a Be-XRB, SXP305 (CXO J005215.4−73191), with an X-ray pulse period of 305.69 ± 0.16 seconds and a likely orbital period of ∼1160-1180 days. Bright sources ( 5 × 10 36 erg s −1 ) in our sample have compact-object classifications consistent with their previously reported types in the literature. Lower luminosity sources ( 5 × 10 36 erg s −1 ) have X-ray colors and luminosities consistent with multiple classifications. We raise questions about possible spectral differences at low luminosity between SMC pulsars and the Galactic pulsars used to create the diagnostic diagrams.

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Section: Source 1745 -Low Luminosity Be-xrbmentioning

confidence: 99%

Neutron Stars and Black Holes in the Small Magellanic Cloud: The SMC NuSTAR Legacy Survey

Lazzarini

Williams

Hornschemeier

et al. 2019

ApJ

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“…Component 1 is the SNR B0057 − 724, identified in radio (Ye et al 1991) and Hα echelle observations (Chu & Kennicutt 1988). It was subsequently detected in several uv absorption lines (Hoopes et al 2001;Koenigsberger et al 2001), and in X-ray images [ROSAT-PSPC (Position Sensitive Proportional Counter); Haberl & Sasaki 2000, and references therein]. Nazé et al (2002) found the remnant to be more or less rectangular using Chandra data with dimensions of 130 × 100 arcsec 2 (41 × 32 pc 2 ).…”

Section: N D I V I D Ua L C O M P O N E N T S I N N 6mentioning

confidence: 99%

“…This SNR was reported as 'component 1' by Ye et al (1991) at α = 00 h 58 m 00 s and δ = −72 • 11 01 . It is identified as RX-J 2 X-ray catalogue number 165 (Haberl & Sasaki 2000). There is also a soft X-ray source, IKT 15, located at α = 00 h 57 m 37 s and δ = −72 • 13 47 (Inoue et al 1983) near its southern edge.…”

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confidence: 99%

An ATCA radio-continuum study of the Small Magellanic Cloud - IV. A multifrequency analysis of the N 66 region

Reid¹,

Payne²,

Filipović³

et al. 2006

Monthly Notices of the Royal Astronomical Society

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Traditional identification of supernova remnants (SNRs) include the use of radio spectral index, optical spectral studies (including strong [S ii], [N ii], [O i], [O ii] and [O iii] lines) and X‐ray co‐identifications. Each of these can have significant limitations within the context of a particular SNR candidate and new identification methods are continually sought. In this paper, we explore subtraction techniques by Ye, Turtle and Kennicutt to remove thermal emission estimated from Hα flux from radio‐continuum images. The remaining non‐thermal emission allows the identification of SNRs embedded within these H ii regions. Subtraction images of the N 66 region in the Small Magellanic Cloud (SMC) using Hα wide‐field optical CCD images from the Curtis Schmidt Telescope and the recent Australia Telescope Compact Array (ATCA)/Parkes radio‐continuum (1420, 2370, 4800 and 8640 MHz) data are presented as an example. These show three SNRs (B0057 − 724, B0056 − 724 and B0056 − 725) separated from their surrounding H ii radio emission. 2.3‐m dual‐beam spectrograph long‐slit spectra from selected regions within N 66 suggest the presence of an additional SNR with no radio or X‐ray emission. Radio spectral index, [S ii]/Hα ratio and archived Chandra images of N 66 combine to give a more coherent picture of this region, confirming B0057 − 724 as an SNR. The N 66 nebula complex is divided into 10 components, composed separately of these SNRs and H ii regions.

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“…A refined X-ray position published by Kahabka & Pietsch (1996) cast doubt over the true optical counterpart, with more than one star looking possible. It was not until Haberl & Sasaki (2000) improved the ROSAT error circle that the star MA93 506 was identified as the most probable counterpart. The orbital period of SXP 8.80 was found to be 28.0 ± 0.…”

Section: R E S U Lt Smentioning

confidence: 99%

On the orbital parameters of Be/X-ray binaries in the Small Magellanic Cloud

Townsend¹,

Coe²,

Corbet³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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The orbital motion of a neutron star about its optical companion presents a window through which we can study the orbital parameters of that binary system. This has been used extensively in the Milky Way to calculate these parameters for several high‐mass X‐ray binaries. Using several years of Rossi X‐ray Timing Explorer Proportional Counter Array data, we derive the orbital parameters of four Be/X‐ray binary systems in the Small Magellanic Cloud (SMC), increasing the number of systems with orbital solutions by a factor of 3. We find one new orbital period, confirm a second and discuss the parameters with comparison to the Galactic systems. Despite the low metallicity in the SMC, these binary systems sit amongst the Galactic distribution of orbital periods and eccentricities, suggesting that metallicity may not play an important role in the evolution of high‐mass X‐ray binary systems. A plot of orbital period against eccentricity shows that the supergiant, Be and low‐eccentricity OB transient systems occupy separate regions of the parameter space; akin to the separated regions on the Corbet diagram. Using a Spearman’s rank correlation test, we also find a possible correlation between the two parameters. The mass functions, inclinations and orbital semimajor axes are derived for the SMC systems based on the binary parameters and the spectral classification of the optical counterpart. As a by‐product of our work, we present a catalogue of the orbital parameters for every high‐mass X‐ray binary in the Galaxy and Magellanic Clouds for which they are known.

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Peter Weiss's Documentary Theater

Cited by 19 publications

References 0 publications

Neutron Stars and Black Holes in the Small Magellanic Cloud: The SMC NuSTAR Legacy Survey

Neutron Stars and Black Holes in the Small Magellanic Cloud: The SMC NuSTAR Legacy Survey

An ATCA radio-continuum study of the Small Magellanic Cloud - IV. A multifrequency analysis of the N 66 region

On the orbital parameters of Be/X-ray binaries in the Small Magellanic Cloud

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