The Infrared Spectrograph (IRS) on the
                    <i>Spitzer Space Telescope</i>

Houck, J. R.; Roellig, Thomas L.; Cleve, Jeffrey Van; Forrest, W. J.; Herter, T.; Lawrence, C. R.; Matthews, K.; Reitsema, H. J.; Soifer, B. T.; Watson, D. M.; Weedman, D. W.; Huisjen, Marty; Troeltzsch, J.; Barry, D. J.; Bernard─Salas, J.; Blacken, C.; Brandl, Bernhard R.; Charmandaris, V.; Devost, D.; Gull, G. E.; Hall, Peter; Henderson, Christine; Higdon, Sarah J.U.; Pirger, Bruce; Schoenwald, Justin; Sloan, G. C.; Uchida, K. I.; Appleton, P. N.; Armus, L.; Burgdorf, M.; Fajardo-Acosta, S. B.; Grillmair, Carl J.; Ingalls, James G.; Morris, P. W.; Teplitz, Harry I.

doi:10.1086/423134

Cited by 1,380 publications

(546 citation statements)

References 13 publications

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“…Low-resolution (R ≈ 60-127) MIR spectroscopy of SN 2004et covered seven epochs between 294 and 1385 days and was obtained using the short-low (SL; 5.2-14.5 μm) and longlow (LL; 14-38 μm) modules of the Infrared Spectrograph (IRS; Houck et al 2004). The log of observations is given in Table 2.…”

Section: Mid-infrared Spectroscopy Of Sn 2004etmentioning

confidence: 99%

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004et

Kotak

Meikle

Farrah

et al. 2009

ApJ

187

290

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We present mid-infrared (MIR) observations of the Type II-plateau supernova (SN) 2004et, obtained with the Spitzer Space Telescope between 64 and 1406 days past explosion. Late-time optical spectra are also presented. For the period 300-795 days past explosion, we argue that the spectral energy distribution (SED) of SN 2004et comprises (1) a hot component due to emission from optically thick gas, as well as free-bound radiation; (2) a warm component due to newly formed, radioactively heated dust in the ejecta; and (3) a cold component due to an IR echo from the interstellar-medium dust of the host galaxy, NGC 6946. There may also have been a small contribution to the IR SED due to free-free emission from ionized gas in the ejecta. We reveal the first-ever spectroscopic evidence for silicate dust formed in the ejecta of a supernova. This is supported by our detection of a large, but progressively declining, mass of SiO. However, we conclude that the mass of directly detected ejecta dust grew to no more than a few times 10 −4 M . We also provide evidence that the ejecta dust formed in comoving clumps of fixed size. We argue that, after about two years past explosion, the appearance of wide, box-shaped optical line profiles was due to the impact of the ejecta on the progenitor circumstellar medium and that the subsequent formation of a cool, dense shell was responsible for a later rise in the MIR flux. This study demonstrates the rich, multifaceted ways in which a typical core-collapse supernova and its progenitor can produce and/or interact with dust grains. The work presented here adds to the growing number of studies that do not support the contention that SNe are responsible for the large mass of observed dust in high-redshift galaxies.

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Section: Mid-infrared Spectroscopy Of Sn 2004etmentioning

confidence: 99%

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004et

Kotak

Meikle

Farrah

et al. 2009

ApJ

187

290

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“…In this paper, we present the mid-infrared (MIR) spectra for 244 galaxy nuclei in the 202 nearby GOALS U/LIRG systems taken with the low resolution module on the Spitzer IRS (Houck et al 2004). The MIR properties derived directly from such a large, complete sample of LIRG spectra will allow us to place these intermediate-luminosity systems into the context of both the extensive previous local ULIRG studies as well as those for lower luminosity star-forming or starbursting systems (Brandl et al 2006;Smith et al 2007b;O'Dowd et al 2009;Wu et al 2010).…”

Section: Introductionmentioning

confidence: 99%

MID-INFRARED PROPERTIES OF NEARBY LUMINOUS INFRARED GALAXIES. I. SPITZER INFRARED SPECTROGRAPH SPECTRA FOR THE GOALS SAMPLE

Stierwalt

Armus

Surace

et al. 2013

ApJS

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192

392

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The Great Observatories All-Sky LIRG Survey (GOALS) is a comprehensive, multiwavelength study of luminous infrared galaxies (LIRGs) in the local universe. Here we present low resolution Spitzer Infrared Spectrograph spectra covering 5-38 μm and provide a basic analysis of the mid-IR spectral properties observed for nearby LIRGs. In a companion paper, we discuss detailed fits to the spectra and compare the LIRGs to other classes of galaxies. The GOALS sample of 244 nuclei in 180 luminous (10 11 L IR /L < 10 12 ) and 22 ultraluminous (L IR /L 10 12 ) IR galaxies represents a complete subset of the IRAS Revised Bright Galaxy Sample and covers a range of merger stages, morphologies, and spectral types. The majority (>60%) of the GOALS LIRGs have high 6.2 μm polycyclic aromatic hydrocarbon (PAH) equivalent widths (EQW 6.2 μm > 0.4 μm) and low levels of silicate absorption (s 9.7 μm > −1.0). There is a general trend among the U/LIRGs for both silicate depth and mid-infrared (MIR) slope to increase with increasing L IR . U/LIRGs in the late to final stages of a merger also have, on average, steeper MIR slopes and higher levels of dust obscuration. Together, these trends suggest that as gas and dust is funneled toward the center of a coalescing merger, the nuclei become more compact and more obscured. As a result, the dust temperature increases also leading to a steeper MIR slope. The sources that depart from these correlations have very low PAH equivalent width (EQW 6.2 μm < 0.1 μm) consistent with their emission being dominated by an active galactic nucleus (AGN) in the MIR. These extremely low PAH EQW sources separate into two distinct types: relatively unobscured sources with a very hot dust component (and thus very shallow MIR slopes) and heavily dust obscured nuclei with a steep temperature gradient. The most heavily dust obscured sources are also the most compact in their MIR emission, suggesting that the obscuring (cool) dust is associated with the outer regions of the starburst and not simply a measure of the dust along the line of sight through a large, dusty disk. A marked decline is seen for the fraction of high EQW (star formation dominated) sources as the merger progresses. The decline is accompanied by an increase in the fraction of composite sources while the fraction of sources where an AGN dominates the MIR emission remains low. When compared to the MIR spectra of submillimeter galaxies (SMGs) at z ∼ 2, both the average GOALS LIRG and ULIRG spectra are more absorbed at 9.7 μm and the average GOALS LIRG has more PAH emission. However, when the AGN contributions to both the local GOALS LIRGs and the high-z SMGs are removed, the average local starbursting LIRG closely resembles the starburst-dominated SMGs.

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“…This estimated value is based on the performance of spectrometers such as Z-spec and IRS on Spitzer, which are similar to the BLISS spectrometer modules. 2,3 The 5σ-2hour line sensitivity is 10 -20 W /m 2 for all 6 bands, assuming a detector NEP of 5x10 -20 W /Hz 1/2 .…”

Section: Expected Photon Noise For Bliss On Spicamentioning

confidence: 99%

Development of fast, background-limited transition-edge sensors for the background-limited infrared/sub-mm spectrograph (BLISS) for SPICA

et al. 2012

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We report experimental progress toward demonstrating background-limited arrays of membrane-isolated transition-edge sensors (TESs) for the Background Limited Infrared/Sub-mm Spectrograph (BLISS). BLISS is a space-borne instrument with grating spectrometers for wavelengths λ= 35-435µm and with R=λ/Δλ~500. The goals for BLISS TESs are: noise equivalent power (NEP) = 5×10-20 W/Hz 1/2 and response time τ<30ms. We expect background-limited performance from bilayers TESs with T C =65mK and G=15fW/K. However, such TESs cannot be operated at 50mK unless stray power on the devices, or dark power P D , is less than 200aW. We describe criteria for measuring P D that requires accurate knowledge of T C. Ultimately, we fabricated superconducting thermistors from Ir (T C ≥135mK) and Mo/Cu proximitized bilayers, where T C is the thermistor transition temperature. We measured the Ir TES arrays in our 45mK base temperature adiabatic demagnetization refrigerator test system, which can measure up to eight 1x32 arrays simultaneously using a time-division multiplexer, as well as our single-pixel test system which can measure down to 15mK. In our previous Ir array measurements our best reported performance was NEP=2.5×10-19 W/Hz

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The Infrared Spectrograph (IRS) on the Spitzer Space Telescope

Cited by 1,380 publications

References 13 publications

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004et

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004et

MID-INFRARED PROPERTIES OF NEARBY LUMINOUS INFRARED GALAXIES. I. SPITZER INFRARED SPECTROGRAPH SPECTRA FOR THE GOALS SAMPLE

Development of fast, background-limited transition-edge sensors for the background-limited infrared/sub-mm spectrograph (BLISS) for SPICA

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