Detection of a Hot Gaseous Halo Around the Giant Spiral Galaxy NGC 1961

Anderson, Michael E.; Bregman, Joel N.

doi:10.1088/0004-637x/737/1/22

Cited by 162 publications

(172 citation statements)

References 59 publications

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“…The results are consistent with the parametric fit obtained by B13, when rescaled to our fiducial metallicity of 0.2Z , as well as with the much more uncertain profile obtained by Anderson & Bregman (2011). No evidence of a break or a flattening in the profile is seen.…”

Section: Discussionsupporting

confidence: 92%

A deepXMM–Newtonstudy of the hot gaseous halo around NGC 1961

Anderson

Churazov

Bregman

2015

Mon. Not. R. Astron. Soc.

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101

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We examine 11 XMM-Newton observations of the giant spiral galaxy NGC 1961, allowing us to study the hot gaseous halo of a spiral galaxy in unprecedented detail. We perform a spatial and a spectral analysis; with the former, the hot halo is detected to at least 80 kpc and with the latter its properties can be measured in detail up to 42 kpc. We find evidence for a negative gradient in the temperature profile as is common for elliptical galaxies. We measure a rough metallicity profile, which is consistent with being flat at Z ∼ 0.2Z . Converting to this metallicity, the deprojected density profile is consistent with previous parametric fits, with no evidence for a break within 42 kpc (∼0.1R vir ). Extrapolating to the virial radius, we infer a hot halo mass comparable to the stellar mass of the galaxy, and a baryon fraction from the stars and hot gas of around 30%. The cooling time of the hot gas is orders of magnitude longer than the dynamical time, making the hot halo stable against cooling instabilities, and we argue that an extended stream of neutral Hydrogen seen to the NW of this galaxy is instead likely due to accretion from the intergalactic medium. The low metallicity of the hot halo suggests it too was likely accreted. We compare the hot halo of NGC 1961 to hot halos around isolated elliptical galaxies, and show that the total mass determines the hot halo properties better than the stellar mass.

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Section: Discussionsupporting

confidence: 92%

A deepXMM–Newtonstudy of the hot gaseous halo around NGC 1961

Anderson

Churazov

Bregman

2015

Mon. Not. R. Astron. Soc.

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101

118

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“…Consequently, the baryonic fraction of the Milky Way halo is ∼50% of the universal value f b , i.e., half of the baryons must have been expelled from the halo or been prevented from being accreted onto it in the first place. 7 We note that this result is in line with the detection of a diffuse X-ray halo around the giant spiral galaxy NGC 1961 (Anderson & Bregman 2011). The observationally derived mass of the ionized gas within ∼500 kpc is ∼(1-3) × 10 11 M .…”

Section: The Distribution Of Gas In Thesupporting

confidence: 81%

Circum-Galactic Gas and the Isotropic Gamma-Ray Background

Feldmann

Hooper

Gnedin

2012

ApJ

101

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Interactions of cosmic rays with the interstellar medium in the disk of the Milky Way provide the majority of the diffuse gamma-ray emission observed by the Fermi Gamma-ray Space Telescope. In addition to the gas which is densely concentrated along the galactic plane, hydrodynamical simulations and observational evidence favor the presence of a halo of hot (T ∼ 10 6 K) ionized hydrogen (H ii), extending with non-negligible densities out to the virial radius of the Milky Way. We show that cosmic-ray collisions with this circum-galactic gas should be expected to provide on the order of 3%-10% of the observed isotopic gamma-ray background at energies above 1 GeV. In addition, gamma rays originating from the extended H ii halos of other galaxies along a given line of sight should contribute at a similar level.

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“…It is only recently that a breakthrough in the observation of hot haloes around disk galaxies has been made, using Chandra and XMM-Newton to detect the hot halos in a handful of extremely massive, fast rotating spiral galaxies: NGC 1961 (Anderson & Bregman 2011), UGC 12591 (Dai et al 2012), NGC 6753 (Bogdán et al 2013) and NGC 266 (Bogdán et al 2013. For these galaxies, extended soft X-ray emission has been detected out to ∼80 kpc, far outside their optical radii.…”

Section: Introductionmentioning

confidence: 99%

A deep Chandra observation of the hot gaseous halo around a rare, extremely massive and relativistic jet launching spiral galaxy

Walker

Fabian

2015

Monthly Notices of the Royal Astronomical Society

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We present a deep Chandra observation of the extremely massive spiral galaxy 2MASX J23453268-0449256, the first X-ray observation of this very rare system which features the largest known relativistic jets from a spiral galaxy. We detect extended X-ray emission from the hot halo surrounding the galaxy, reaching out to 80 kpc in radius. The hot halo is elongated along the plane of the spiral galaxy, and one possibility is that the powerful relativistic jets have disrupted the hot halo gas located perpendicular to the disk. Our calculations indicate that it is energetically feasible that the AGN feedback in this system could have uplifted or completely expelled a significant fraction of the gas in the 20-80 kpc radial range. We also detect extended emission which appears to be associated with the inner and outer southern radio lobes, and is possibly the result of inverse Compton emission. Using the observed X-ray and radio luminosity of the central AGN, the fundamental plane of Gultekin et al. predicts a black hole mass of 5×10 8 M ⊙ , with a range of 1 × 10 8 -3 × 10 9 M ⊙ when the scatter in the fundamental plane relation is taken into account. This is consistent with the possibility that an exceptionally massive (> 10 9 M ⊙ ) black hole lies at the centre of this galaxy, as suggested by the M BH − σ scaling relation, but a tighter constraint cannot be made.

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Detection of a Hot Gaseous Halo Around the Giant Spiral Galaxy NGC 1961

Cited by 162 publications

References 59 publications

A deepXMM–Newtonstudy of the hot gaseous halo around NGC 1961

A deepXMM–Newtonstudy of the hot gaseous halo around NGC 1961

Circum-Galactic Gas and the Isotropic Gamma-Ray Background

A deep Chandra observation of the hot gaseous halo around a rare, extremely massive and relativistic jet launching spiral galaxy

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