Modeling the Neutral Hydrogen Interstellar Medium: A Better Kinematic Distance Tool

Foster, Tyler; MacWilliams, J.

doi:10.1086/500815

Cited by 53 publications

(63 citation statements)

References 39 publications

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“…The obtained spectra of the shell and the Lobe could be well fitted with a one-component non-equilibrium ionisation (NEI) model, describing a mixture of the shocked ISM and shocked ejecta. The preshock density of the ambient medium was derived to be n 0 = (0.16 ± 0.02) d −0.5 3 cm −3 , where d 3 = D/3.0 kpc is a scaling factor accounting for the distance D of CTB 109, which was estimated as 3.2 ± 0.2 kpc by Kothes & Foster (2012) with the new method of Foster & MacWilliams (2006). This results in a density of the medium of n 0 = 0.155 cm −3 in case of the XMM-Newton data.…”

Section: Model Setupmentioning

confidence: 99%

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

Bolte

Sasaki

Breitschwerdt

2015

A&A

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Context. Using detailed 3D hydrodynamic simulations we study the nature of the Galactic supernova remnant (SNR) CTB 109 (G109.1-1.0), which is well known for its semicircular shape and a bright diffuse X-ray emission feature inside the SNR. Aims. Our model has been designed to explain the observed morphology, with a special emphasis on the bright emission feature inside the SNR. Moreover, we determine the age of the remnant and compare our findings with X-ray observations. With CTB 109 we test a new method of detailed numerical simulations of diffuse young objects, using realistic initial conditions derived directly from observations. Methods. We performed numerical 3D simulations with the RAMSES code. The initial density structure has been directly taken from 12 CO emission data, adding an additional dense cloud, which, when it is shocked, causes the bright emission feature.Results. From parameter studies we obtained the position ( , b) = (109.1545 • , −1.0078 • ) for an elliptical cloud with n cloud = 25 cm −3 based on the preshock density from Chandra data and a maximum diameter of 4.54 pc, whose encounter with the supernova (SN) shock wave generates the bright X-ray emission inside the SNR. The calculated age of the remnant is about 11 000 yr according to our simulations. In addition, we can also determine the most probable site of the SN explosion. Conclusions. Hydrodynamic simulations can reproduce the morphology and the observed size of the SNR CTB 109 remarkably well. Moreover, the simulations show that it is very plausible that the bright X-ray emission inside the SNR is the result of an elliptical dense cloud shocked by the SN explosion wave. We show that numerical simulations using observational data for an initial model can produce meaningful results.

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Section: Model Setupmentioning

confidence: 99%

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

Bolte

Sasaki

Breitschwerdt

2015

A&A

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“…Indeed, using a new method (Foster & MacWilliams 2006 to extrapolate their velocity-distance relation to obtain a distance estimate of approximately 11.5 kpc for GSH 91.5+2−114. This slightly lower distance still corresponds to an object well in the outer Galaxy at R g ≈ 14.5 kpc and z ∼ 400 pc.…”

Section: Discussionmentioning

confidence: 99%

GSH 91.5+2–114: A large H i shell in the outer part of the Galaxy

Cichowolski

Pineault

2010

A&A

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GSH 91.5 + 2 − 114 is a large H i shell located in the outer Galaxy at a kinematic distance of about 15 kpc. It was first identified in the Canadian Galactic Plane Survey (CGPS) by Pineault et al. (2002, ASP Conf. Ser., 276, 332) as being possibly associated with objects possessing infrared colors, which indicates strong stellar winds. The H i shell has no obvious continuum counterpart in the CGPS radio images at 408 and 1420 MHz or in the IRAS images. We found no evidence for early-type massive stars, most likely as a result of the large extinction that is expected for this large distance. An analysis of the energetics and of the main physical parameters of the H i shell shows that this shell is likely the result of the combined action of the stellar winds and supernova explosions of many stars. We investigate whether a number of slightly extended regions characterized by a thermal radio continuum and located near the periphery of the H i shell could be the result of star formation triggered by the expanding shell.

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“…Roberts (1972) identifies different zones in a velocity-distance diagram that describes the kinematics in the direction of the Perseus arm: a shock jump, a region of dense gas behind the shock, a velocity "hill", and a velocity trough on the location of a local gas density peak. Foster & MacWilliams (2006) developed another method to deal with distances in the direction of the Perseus arm. The method uses an empirical fitting of HI fluxes in order to find distances along the Perseus arm direction.…”

Section: Previous Distance Estimatesmentioning

confidence: 99%

Kinematics of the Galactic Supernova Remnant G109.1-1.0 (CTB 109)

Sánchez-Cruces

Rosado

Fuentes-Carrera

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present direct images in the Hα and [SII]λλ6717,6731Å lines of the Galactic Supernova Remnant G109.1-1.0 (CTB 109). We confirm that the filaments detected are the optical counterpart of the X-ray and radio supernova remnant due to their high [SII]/Hα line-ratios. We study for the first time the kinematics of the optical counterpart of SNR CTB 109 using the UNAM scanning Fabry-Perot interferometer PUMA. We estimate a systemic velocity of V LSR =-50±6 km s −1 for this remnant and an expansion velocity of V exp =230±5 km s −1 . From this velocity value and taking into account previous studies about the kinematics of objects at that Galactic longitude we derive a distance to the SNR CTB 109 of 3.1±0.2 kpc, locating it in the Perseus arm. Using the [SII]λ6717/[SII]λ6731 line-ratio we find an electronic density value around n e = 580 cm −3 . Considering that this remnant is evolving in a low density medium with higher density cloudlets responsible of the optical emission, we determine the age and energy deposited in the ISM by the supernova explosion (E 0 ) in both the Sedov-Taylor phase and the radiative phase. For both cases the age is of thousands of years and the E 0 is rather typical of SNRs containing simple pulsars so that, the energy released to the ISM cannot be used to distinguish between supernova remnants hosting typical pulsars from those hosting powerful magnetars as in the case of CTB 109.

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Modeling the Neutral Hydrogen Interstellar Medium: A Better Kinematic Distance Tool

Cited by 53 publications

References 39 publications

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

3D hydrodynamic simulations of the Galactic supernova remnant CTB 109

GSH 91.5+2–114: A large H i shell in the outer part of the Galaxy

Kinematics of the Galactic Supernova Remnant G109.1-1.0 (CTB 109)

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