A downward revision to the distance of the 1806−20 cluster and associated magnetar from Gemini Near-Infrared Spectroscopy

Bibby, Joanne; Crowther, P. A.; Furness, J. P.; Clark, J. S.

doi:10.1111/j.1745-3933.2008.00453.x

Cited by 114 publications

(127 citation statements)

References 28 publications

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“…Different physical mechanisms can generate similar H−K s and J − H colors; LBVs have J−K s colors from ∼1.0 to ∼5.0 mag, and H−K s from ∼0.2 mag to ∼2.0 mag. A sample of five LBVs (AFGL2298, Pistol Star, WR102ka, LBV1806−20, G0.120−0.048, FMM362) have redder J−K s , which are consistent with distant sources at large interstellar extinction (A K s = 3.15, 2.99, 2.78, 3.0, 3.26, 3.42 mag, respectively Clark et al 2003;Mauerhan et al 2010;Barniske et al 2008;Bibby et al 2008).…”

Section: H-k S Versus J-h Diagrammentioning

confidence: 79%

Near- and mid-infrared colors of evolved stars in the Galactic plane. TheQ1 andQ2 parameters

Messineo

Menten

Churchwell

et al. 2011

A&A

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Context. Mass-loss from evolved stars chemically enriches the interstellar medium (ISM). Stellar winds from massive stars and their explosions as supernovae shape the ISM and trigger star formation. Studying evolved stars is fundamental for understanding galaxy formation and evolution at any redshift. Aims. We aim to establish a photometric classification scheme for Galactic mass-losing evolved stars (e.g., WR, RSG, and AGB stars) with the goal of identifying new ones, and subsequently to use these samples as tracers of Galactic structure. Methods. We searched for counterparts of known Galactic WR, LBV, RSG, and O-rich AGB stars in the 2MASS, GLIMPSE, and MSX catalogs, and we analyzed their properties with near-and mid-infrared color-color diagrams. Results. We used the Q1 parameter, which is a measure of the deviation from the interstellar reddening vector in the J − H versus H−K s diagram, and we defined a new parameter, Q2, which is a measure of the deviation from the interstellar reddening vector in the Conclusions. The GLIMPSE catalog is a powerful tool for photometric classification of Galactic mass-losing evolved stars. Our new criteria will yield many new RSGs and WRs.

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Section: H-k S Versus J-h Diagrammentioning

confidence: 79%

Near- and mid-infrared colors of evolved stars in the Galactic plane. TheQ1 andQ2 parameters

Messineo

Menten

Churchwell

et al. 2011

A&A

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“…(1) Bibby et al 2008; (2) Kouveliotou et al 1998; (3) Kouveliotou et al 1999. shown that the effects of mass transfer onto a companion star significantly reduce the RSG lifetime (Eldridge et al 2008). This enables the core to retain angular momentum through to SN, enough perhaps to greatly amplify the resulting neutron star's magnetic field through the dynamo mechanism in the first few seconds of its life.…”

Section: The Possible Role Of Binaritymentioning

confidence: 99%

The Progenitor Mass of the Magnetar Sgr1900+14

Davies

Figer

Kudritzki

et al. 2009

ApJ

100

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Magnetars are young neutron stars with extreme magnetic fields (B 10 14 -10 15 G). How these fields relate to the properties of their progenitor stars is not yet clearly established. However, from the few objects associated with young clusters it has been possible to estimate the initial masses of the progenitors, with results indicating that a very massive progenitor star (M prog > 40 M ) is required to produce a magnetar. Here, we present adaptive-optics assisted Keck/ NIRC2 imaging and Keck/NIRSPEC spectroscopy of the cluster associated with the magnetar SGR 1900+14, and report that the initial progenitor star mass of the magnetar was a factor of 2 lower than this limit, M prog = 17±2 M . Our result presents a strong challenge to the concept that magnetars can only result from very massive progenitors. Instead, we favor a mechanism which is dependent on more than just initial stellar mass for the production of these extreme magnetic fields, such as the "fossil-field" model or a process involving close binary evolution.

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“…This leads to L PL X = 4.1×10 35 erg s −1 . If we use instead the revised distance of 8.7 kpc (Bibby et al 2008), we have L PL X = 1.4 × 10 35 erg s −1 . Figure 7 shows the ratio L PL X /Ė rot as a function of the NS mass in the case of SGR 1900+14 and SGR 1806-20, adopting the GM1 EOS and assuming a distance of 15 kpc for both sources.…”

Section: Sgrs and Axps Efficiencymentioning

confidence: 99%

The rotation-powered nature of some soft gamma-ray repeaters and anomalous X-ray pulsars

Coelho

Cáceres

Lima

et al. 2017

A&A

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Context. Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are slow rotating isolated pulsars whose energy reservoir is still matter of debate. Adopting neutron star (NS) fiducial parameters; mass M = 1.4M , radius R = 10 km, and moment of inertia, I = 10 45 g cm 2 , the rotational energy loss,Ė rot , is lower than the observed luminosity (dominated by the X-rays) L X for many of the sources. Aims. We investigate the possibility that some members of this family could be canonical rotation-powered pulsars using realistic NS structure parameters instead of fiducial values. Methods. We compute the NS mass, radius, moment of inertia and angular momentum from numerical integration of the axisymmetric general relativistic equations of equilibrium. We then compute the entire range of allowed values of the rotational energy loss,Ė rot , for the observed values of rotation period P and spin-down rateṖ. We also estimate the surface magnetic field using a general relativistic model of a rotating magnetic dipole. Results. We show that realistic NS parameters lowers the estimated value of the magnetic field and radiation efficiency, L X /Ė rot , with respect to estimates based on fiducial NS parameters. We show that nine SGRs/AXPs can be described as canonical pulsars driven by the NS rotational energy, for L X computed in the soft (2-10 keV) X-ray band. We compute the range of NS masses for which L X /Ė rot < 1. We discuss the observed hard X-ray emission in three sources of the group of nine potentially rotation-powered NSs. This additional hard X-ray component dominates over the soft one leading to L X /Ė rot > 1 in two of them. Conclusions. We show that 9 SGRs/AXPs can be rotation-powered NSs if we analyze their X-ray luminosity in the soft 2-10 keV band. Interestingly, four of them show radio emission and six have been associated with supernova remnants (including Swift J1834.9-0846 the first SGR observed with a surrounding wind nebula). These observations give additional support to our results of a natural explanation of these sources in terms of ordinary pulsars. Including the hard X-ray emission observed in three sources of the group of potential rotation-powered NSs, this number of sources with L X /Ė rot < 1 becomes seven. It remains open to verification 1) the accuracy of the estimated distances and 2) the possible contribution of the associated supernova remnants to the hard X-ray emission.

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A downward revision to the distance of the 1806−20 cluster and associated magnetar from Gemini Near-Infrared Spectroscopy

Cited by 114 publications

References 28 publications

Near- and mid-infrared colors of evolved stars in the Galactic plane. TheQ1 andQ2 parameters

Near- and mid-infrared colors of evolved stars in the Galactic plane. TheQ1 andQ2 parameters

The Progenitor Mass of the Magnetar Sgr1900+14

The rotation-powered nature of some soft gamma-ray repeaters and anomalous X-ray pulsars

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