Observations of the Galactic Nucleus at 350 Microns

Gezari, D. Y.; Joyce, R. R.; Simón, M.

doi:10.1086/181118

Cited by 28 publications

(22 citation statements)

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“…Aside from the extreme luminosity, SN 2008es is of great interest since detailed ultraviolet (UV) through infrared (IR) observations provide a unique opportunity to study the mass-loss properties of an evolved post-main sequence massive star via its interaction with the surrounding dense CSM. A similar analysis of SN 2008es has been presented by Gezari et al (2008b).…”

Section: Introductionsupporting

confidence: 70%

“…The temperature and luminosity decrease while the radius increases with time, as expected for an expanding and cooling SN photosphere. In order to determine the time of V -band maximum light, which at the redshift of this SN roughly corresponds to rest-frame B, we convert the early time g, r, and i ′ photometry taken with the Palomar 1.5-m telescope from Gezari et al (2008b) to V RI using the color equations from Jester et al (2005). Following a quadratic fit to these data, we find that the observed V -band maximum occurred on ∼2008 May 13, ∼15 restframe days after discovery.…”

Section: Photometric Resultsmentioning

confidence: 99%

“…We Gezari et al 2008b), as well as our optical-NIR observations (filled symbols; KAIT, Nickel, PFCam, and PAIRITEL) and space-based UVOT observations from Swift (filled triangles). We adopt the discovery date of SN 2008es, 2008 Apr.…”

Section: Observationsmentioning

confidence: 99%

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THE EXCEPTIONALLY LUMINOUS TYPE II-LINEAR SUPERNOVA 2008es

Miller

Chornock

Perley

et al. 2008

ApJ

155

230

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We report on our early photometric and spectroscopic observations of the extremely luminous Type II supernova (SN) 2008es. With an observed peak optical magnitude of m V = 17.8 and at a redshift z = 0.213, SN 2008es had a peak absolute magnitude of M V = −22.3, making it the second most luminous SN ever observed. The photometric evolution of SN 2008es exhibits a fast decline rate (∼0.042 mag d −1 ), similar to the extremely luminous Type II-L SN 2005ap. We show that SN 2008es spectroscopically resembles the luminous Type II-L SN 1979C. Although the spectra of SN 2008es lack the narrow and intermediate-width line emission typically associated with the interaction of a SN with the circumstellar medium of its progenitor star, we argue that the extreme luminosity of SN 2008es is powered via strong interaction with a dense, optically thick circumstellar medium. The integrated bolometric luminosity of SN 2008es yields a total radiated energy at ultraviolet and optical wavelengths of 10 51 ergs. Finally, we examine the apparently anomalous rate at which the Texas Supernova Search has discovered rare kinds of supernovae, including the five most luminous supernovae observed to date, and find that their results are consistent with those of other modern SN searches.

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Section: Introductionsupporting

confidence: 70%

Section: Photometric Resultsmentioning

confidence: 99%

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THE EXCEPTIONALLY LUMINOUS TYPE II-LINEAR SUPERNOVA 2008es

Miller

Chornock

Perley

et al. 2008

ApJ

155

230

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“…The shape of the MBB component is calculated using the ratio of the 70 and 160 µm fluxes to numerically derive a temperature of the dust 15 , and a β = 2. We choose the classical emissivity index of β = 2 (Gezari et al 1973;Draine & Lee 1984) for simplicity. The emissivity index depends upon the chemical nature and internal physics of the grains and is generally thought to be from 1 ≤ β ≤ 2 (Dupac et al 2003) with some indications that it can be greater than two (Mennella et al 1998;Désert et al 2008).…”

Section: Tirmentioning

confidence: 99%

SPITZERANALYSIS OF H II REGION COMPLEXES IN THE MAGELLANIC CLOUDS: DETERMINING A SUITABLE MONOCHROMATIC OBSCURED STAR FORMATION INDICATOR

Lawton¹,

Gordon²,

Babler³

et al. 2010

ApJ

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H II regions are the birth places of stars, and as such they provide the best measure of current star formation rates (SFRs) in galaxies. The close proximity of the Magellanic Clouds allows us to probe the nature of these star forming regions at small spatial scales. To study the H II regions, we compute the bolometric infrared flux, or total infrared (TIR), by integrating the flux from 8 to 500 µm. The TIR provides a measure of the obscured star formation because the UV photons from hot young stars are absorbed by dust and re-emitted across the mid-to-far-infrared (IR) spectrum. We aim to determine the monochromatic IR band that most accurately traces the TIR and produces an accurate obscured SFR over large spatial scales. We present the spatial analysis, via aperture/annulus photometry, of 16 Large Magellanic Cloud (LMC) and 16 Small Magellanic Cloud (SMC) H II region complexes using the Spitzer Space Telescope's IRAC (3.6, 4.5, 8 µm) and MIPS (24, 70, 160 µm) bands. Ultraviolet rocket data (1500 and 1900 Å) and SHASSA Hα data are also included. All data are convolved to the MIPS 160 µm resolution (40 arcsec full width at half-maximum), and apertures have a minimum radius of 35 ′′ . The IRAC, MIPS, UV, and Hα spatial analysis are compared with the spatial analysis of the TIR. We find that nearly all of the LMC and SMC H II region spectral energy distributions (SEDs) peak around 70 µm at all radii, from ∼ 10 to ∼ 400 pc from the central ionizing sources. As a result, we find the following: the sizes of H II regions as probed by 70 µm is approximately equal to the sizes as probed by TIR (≈ 70 pc in radius); the radial profile of the 70 µm flux, normalized by TIR, is constant at all radii (70 µm ∼ 0.45 TIR); the 1σ standard deviation of the 70 µm fluxes, normalized by TIR, is a lower fraction of the mean (0.05 − 0.12 out to ∼ 220 pc) than the normalized 8, 24, and 160 µm normalized fluxes (0.12 − 0.52); and these results are the same for the LMC and the SMC. From these results, we argue that 70 µm is the most suitable IR band to use as a monochromatic obscured star formation indicator because it most accurately reproduces the TIR of H II regions in the LMC and SMC and over large spatial scales. We also explore the general trends of the 8, 24, 70, and 160 µm bands in the LMC and SMC H II region SEDs, radial surface brightness profiles, sizes, and normalized (by TIR) radial flux profiles. We derive an obscured SFR equation that is modified from the literature to use 70 µm luminosity, SFR (M ⊙ yr −1 ) = 9.7(0.7) × 10 −44 L 70 (ergs s −1 ), which is applicable from 10 to 300 pc distance from the center of an H II region. We include an analysis of the spatial variations around H II regions between the obscured star formation indicators given by the IR and the unobscured star formation indicators given by UV and Hα. We compute obscured and unobscured SFRs using equations from the literature and examine the spatial variations of the SFRs around H II regions.

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“…A classical value is 2, following the investigations of Gezari et al (1973) and the calculations of, for instance, Draine & Lee (1984). This value is particularly invoked for isotropic crystalline grains, and it is thought to be an upper limit (Wooten 1972;Emerson 1988).…”

Section: Introductionmentioning

confidence: 99%

Inverse temperature dependence of the dust submillimeter spectral index

Dupac

Bernard

Boudet

et al. 2003

A&A

259

349

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Abstract. We present a compilation of PRONAOS-based results concerning the temperature dependence of the dust submillimeter spectral index, including data from Galactic cirrus, star-forming regions, dust associated to a young stellar object, and a spiral galaxy. We observe large variations of the spectral index (from 0.8 to 2.4) in a wide range of temperatures (11 to 80 K). These spectral index variations follow a hyperbolic-shaped function of the temperature, high spectral indices (1.6-2.4) being observed in cold regions (11-20 K) while low indices (0.8-1.6) are observed in warm regions (35-80 K). Three distinct effects may play a role in this temperature dependence: one is that the grain sizes change in dense environments, another is that the chemical composition of the grains is not the same in different environments, a third one is that there is an intrinsic dependence of the dust spectral index on the temperature due to quantum processes. This last effect is backed up by laboratory measurements and could be the dominant one.

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Observations of the Galactic Nucleus at 350 Microns

Cited by 28 publications

References 0 publications

THE EXCEPTIONALLY LUMINOUS TYPE II-LINEAR SUPERNOVA 2008es

THE EXCEPTIONALLY LUMINOUS TYPE II-LINEAR SUPERNOVA 2008es

SPITZERANALYSIS OF H II REGION COMPLEXES IN THE MAGELLANIC CLOUDS: DETERMINING A SUITABLE MONOCHROMATIC OBSCURED STAR FORMATION INDICATOR

Inverse temperature dependence of the dust submillimeter spectral index

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