CASSIS: THE CORNELL ATLAS OF
                    <i>SPITZER</i>
                    /INFRARED SPECTROGRAPH SOURCES

Lebouteiller, V.; Barry, D. J.; Spoon, H. W. W.; Bernard─Salas, J.; Sloan, G. C.; Houck, J. R.; Weedman, D. W.

doi:10.1088/0067-0049/196/1/8

Cited by 315 publications

(319 citation statements)

References 16 publications

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“…The IRS line fluxes are provided in Appendix C. We provide in the following some details on the spectral extraction. The low-resolution data were retrieved from the CASSIS spectral database v6 (Lebouteiller et al 2011). For pointsources, we used the optimal extraction spectra, which provide the best S/N.…”

Section: Additional Sources Of Uncertaintymentioning

confidence: 99%

TheHerschelDwarf Galaxy Survey

Cormier

Madden

Lebouteiller

et al. 2015

A&A

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234

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Context. The far-infrared (FIR) lines are important tracers of the cooling and physical conditions of the interstellar medium (ISM) and are rapidly becoming workhorse diagnostics for galaxies throughout the universe. There are clear indications of a different behavior of these lines at low metallicity that needs to be explored. Aims. Our goal is to explain the main differences and trends observed in the FIR line emission of dwarf galaxies compared to more metal-rich galaxies, and how this translates in ISM properties. ] 57 µm fine-structure cooling lines in a sample of 48 low-metallicity star-forming galaxies of the guaranteed time key program Dwarf Galaxy Survey. We correlate PACS line ratios and line-to-L TIR ratios with L TIR , L TIR /L B , metallicity, and FIR color, and interpret the observed trends in terms of ISM conditions and phase filling factors with Cloudy radiative transfer models. Results. We find that the FIR lines together account for up to 3 percent of L TIR and that star-forming regions dominate the overall emission in dwarf galaxies. Compared to metal-rich galaxies, the ratios of Harboring compact phases of a low filling factor and a large volume filling factor of diffuse gas, the ISM of low-metallicity dwarf galaxies has a more porous structure than that of metal-rich galaxies. Methods

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Section: Additional Sources Of Uncertaintymentioning

confidence: 99%

TheHerschelDwarf Galaxy Survey

Cormier

Madden

Lebouteiller

et al. 2015

A&A

Self Cite

234

399

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“…Our parent sample is the list of extragalactic sources with Spitzer/IRS spectra in the version 7 of the Cornell Atlas of Spitzer/IRS Sources (CASSIS; Lebouteiller et al 2011Lebouteiller et al , 2015. A careful identification of the optical counterpart was performed as part of the preparation work for the Infrared Database of Extragalactic Observables with Spitzer (IDEOS; Spoon et al in prep.).…”

Section: Sample Selectionmentioning

confidence: 99%

The near-to-mid infrared spectrum of quasars

Hernán-Caballero

Hatziminaoglou

Alonso‐Herrero

et al. 2016

Mon. Not. R. Astron. Soc.

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We analyse a sample of 85 luminous (log(νL ν (3µm)/erg s −1 )>45.5) quasars with restframe ∼2-11 µm spectroscopy from AKARI and Spitzer. Their high luminosity allows a direct determination of the near-infrared quasar spectrum free from host galaxy emission. A semiempirical model consisting of a single template for the accretion disk and two blackbodies for the dust emission successfully reproduces the 0.1-10 µm spectral energy distributions (SEDs). Excess emission at 1-2 µm over the best-fitting model suggests that hotter dust is necessary in addition to the ∼1200 K blackbody and the disk to reproduce the entire near-infrared spectrum. Variation in the extinction affecting the disk and in the relative strength of the disk and dust components accounts for the diversity of individual SEDs. Quasars with higher dust-to-disk luminosity ratios show slightly redder infrared continua and less prominent silicate emission. We find no luminosity dependence in the shape of the average infrared quasar spectrum. We generate a new quasar template that covers the restframe range 0.1-11 µm, and separate templates for the disk and dust components. Comparison with other infrared quasar composites suggests that previous ones are less reliable in the 2-4 µm range. Our template is the first one to provide a detailed view of the infrared emission on both sides of the 4 µm bump.

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“…The first one is the Cornell atlas of Spitzer/IRS spectra (CASSIS 2 ). CASSIS provides low-resolution spectra (R ∼ 60−127 over 5.2 µm to 38 µm) with the IRS instruments in the stare mode (Lebouteiller et al 2011). The second database is the Spitzer infrared nearby galaxy survey (SINGS Kennicutt et al 2003).…”

Section: Samplementioning

confidence: 99%

Nuclear obscuration in LINERs

González‐Martín

Masegosa

Márquez

et al. 2015

A&A

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Context. Most of the optically classified low-ionisation, narrow emission-line regions (LINERs) nuclei host an active galactic nucleus (AGN). However, how they fit into the unified model (UM) of AGN is still an open question.Aims. The aims of this work are to study at mid-infrared (mid-IR) (1) the Compton-thick nature of LINERs (i.e. hydrogen column densities of N H > 1.5 × 10 24 cm −2 ) and (2) the disappearance of the dusty torus in LINERs predicted from theoretical arguments. Methods. We have compiled all the available low spectral-resolution, mid-IR spectra of LINERs from the InfraRed Spectrograph (IRS) onboard Spitzer. The sample contains 40 LINERs. We have complemented the LINER sample with Spitzer/IRS spectra of PG QSOs, Type-1 Seyferts (S1s), Type-2 Seyferts (S2s), and StarBurst (SB) nuclei. We studied the AGN compared to the starburst content in our sample using different indicators: the equivalent width of the polycyclic aromatic hydrocarbon at 6.2 µm, the strength of the silicate feature at 9.7 µm, and the steepness of the mid-IR spectra. We classified the spectra as SB-dominated and AGN-dominated, according to these diagnostics and compared the average mid-IR spectra of the various classes. Moreover, we studied the correlation between the 12 µm luminosity, νL ν (12 µm), and the 2−10 keV energy band X-ray luminosity, L X (2−10 keV). Results. In 25 out of the 40 LINERs (i.e. 62.5%), the mid-IR spectra are not SB-dominated, similar to the comparison S2 sample (67.7%). The average spectra of both SB-dominated LINERs and S2s are very similar to the average spectrum of the SB class. The average spectrum of AGN-dominated LINERs is different from the average spectra of the other optical classes, showing a rather flat spectrum at 6−28 µm. We find that the average spectrum of AGN-dominated LINERs with X-ray luminosities L X (2−10 keV) > 10 41 erg/s is similar to the average mid-IR spectrum of AGN-dominated S2s. However, faint LINERs (i.e. L X (2−10 keV) < 10 41 erg/s) show flat spectra different from any of the other optical classes. The correlation between νL ν (12 µm) and L X (2−10 keV) for AGN nicely extends towards low luminosities only if SB-dominated LINERs are excluded and if the 2−10 keV band X-ray luminosity is corrected in Compton-thick LINER candidates. Conclusions. We find that LINERs proposed as Compton-thick candidates at X-ray wavelengths may be confirmed according to the X-ray to mid-IR luminosity relation. We show evidence that the dusty-torus disappear when their bolometric luminosity is below L bol 10 42 erg/s. We suggest that the dominant emission at mid-IR of faint LINERs might be a combination of an elliptical galaxy host (characterised by the lack of gas), a starburst, a jet, and/or ADAF emission. Alternatively, the mid-IR emission of some of these faint LINERs could be a combination of elliptical galaxy plus carbon-rich planetary nebulae. To reconcile the Compton-thick nature of a large number of LINERs without dusty-torus signatures, we suggest that the material producing the ...

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CASSIS: THE CORNELL ATLAS OF SPITZER /INFRARED SPECTROGRAPH SOURCES

Cited by 315 publications

References 16 publications

TheHerschelDwarf Galaxy Survey

TheHerschelDwarf Galaxy Survey

The near-to-mid infrared spectrum of quasars

Nuclear obscuration in LINERs

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