Calibration and Performance of the ISO Long-Wavelength Spectrometer

Armand, Céline; Burgdorf, M.; Caux, E.; Ceccarelli, C.; Colgan, Sean W. J.; Cruvellier, P.; Fischer, J.; Furniss, I.; Greenhouse, Matthew A.; Molinari, S.; Orfei, R.; Pequignot, D.; Saïsse, M.; Saraceno, P.; Serra, G.; Spinoglio, L.

doi:10.21236/ada464476

Cited by 114 publications

(143 citation statements)

References 4 publications

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“…The sample was observed by Herschel using the Spectral and Photometric Imaging REceiver (SPIRE, Griffin et al 2010) in both photometry (250, 350, 500 μm) and spectroscopy using the SPIRE Fourier Transform Spectrometer, (FTS; Swinyard et al 2010) from 194 to 671 μm (except 3C273, which only has photometric data). The SPIRE photometry and spectroscopy observations were carried out between 2011 July 26th (Herschel Operational Day, OD804) and 2012 October 19th (OD 1178).…”

Section: Observationsmentioning

confidence: 99%

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Pearson¹,

Rigopoulou²,

Hurley³

et al. 2016

ApJS

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We present the Herschel SPIRE Fourier Transform Spectroscopy (FTS) atlas for a complete flux-limited sample of local ultraluminous infrared galaxies (ULIRGs) as part of the HERschel Ultra Luminous InfraRed Galaxy Survey (HERUS). The data reduction is described in detail and was optimized for faint FTS sources ,with particular care being taken for the subtraction of the background, which dominates the continuum shape of the spectra. To improve the final spectra, special treatment in the data reduction has been given to any observation suffering from artifacts in the data caused by anomalous instrumental effects. Complete spectra are shown covering 200-671 μm, with photometry in the SPIRE bands at 250, 350, and 500 μm. The spectra include near complete CO ladders for over half of our sample, as well as fine structure lines from [C I] 370 μm, [C I] 609 μm, and [N II] 205 μm. We also detect H 2 O lines in several objects. We construct CO spectral line energy distributions (SLEDs) for the sample, and compare their slopes with the far-infrared (FIR) colors and luminosities. We show that the CO SLEDs of ULIRGs can be broadly grouped into three classes based on their excitation. We find that the mid-J (5<J<8) lines are better correlated with the total FIR luminosity, suggesting that the warm gas component is closely linked to recent star formation. The higher J transitions do not linearly correlate with the FIR luminosity, consistent with them originating in hotter, denser gas that is unconnected to the current star formation. We conclude that in most cases more than one temperature component is required to model the CO SLEDs.

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Section: Observationsmentioning

confidence: 99%

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Pearson¹,

Rigopoulou²,

Hurley³

et al. 2016

ApJS

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“…The measured fluxes are listed in Table 1. The absolute flux calibration is 2 and 5% for MIPS 24 and 70 μm bands and is 20% for PACS (Poglitsch et al 2010) and 15% for SPIRE (Swinyard et al 2010), respectively. We adopted these values as the flux density uncertainty for these bands.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Dust in the bright supernova remnant N49 in the LMC

Otsuka¹,

Loon

Long³

et al. 2010

A&A

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We investigate the dust associated with the supernova remnant (SNR) N49 in the Large Magellanic Cloud (LMC) as observed with the Herschel Space Observatory. N49 is unusually bright because of an interaction with a molecular cloud along its eastern edge. We have used PACS and SPIRE to measure the far IR flux densities of the entire SNR and of a bright region on the eastern edge of the SNR where the SNR shock is encountering the molecular cloud. Using these fluxes supplemented with archival data at shorter wavelengths, we estimate the dust mass associated with N49 to be about 10 M . The bulk of the dust in our simple two-component model has a temperature of 20-30 K, similar to that of nearby molecular clouds. Unfortunately, as a result of the limited angular resolution of Herschel at the wavelengths sampled with SPIRE, the uncertainties are fairly large. Assuming this estimate of the dust mass associated with the SNR is approximately correct, it is probable that most of the dust in the SNR arises from regions where the shock speed is too low to produce significant X-ray emission. The total amount of warm 50-60 K dust is ∼0.1 or 0.4 M , depending on whether the dust is modeled in terms of carbonaceous or silicate grains. This provides a firm lower limit to the amount of shock heated dust in N49.

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“…The PACS instrument is described by Poglitsch et al (2010). The SPIRE instrument, its in-orbit performance, and its scientific capabilities are described by Griffin et al (2010), and the SPIRE astronomical calibration methods and accuracy are outlined by Swinyard et al (2010). The reduction of our data is described in Appendix A.…”

Section: Observationsmentioning

confidence: 99%

Herschelimages of NGC 6720: H₂formation on dust grains

Hoof

Steene

Barlow

et al. 2010

A&A

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Herschel PACS and SPIRE images have been obtained of NGC 6720 (the Ring nebula). This is an evolved planetary nebula with a central star that is currently on the cooling track, due to which the outer parts of the nebula are recombining. From the PACS and SPIRE images we conclude that there is a striking resemblance between the dust distribution and the H 2 emission, which appears to be observational evidence that H 2 forms on grain surfaces. We have developed a photoionization model of the nebula with the Cloudy code which we used to determine the physical conditions of the dust and investigate possible formation scenarios for the H 2 . We conclude that the most plausible scenario is that the H 2 resides in high density knots which were formed after the recombination of the gas started when the central star entered the cooling track. Hydrodynamical instabilities due to the unusually low temperature of the recombining gas are proposed as a mechanism for forming the knots. H 2 formation in the knots is expected to be substantial after the central star underwent a strong drop in luminosity about one to two thousand years ago, and may still be ongoing at this moment, depending on the density of the knots and the properties of the grains in the knots.

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Calibration and Performance of the ISO Long-Wavelength Spectrometer

Cited by 114 publications

References 4 publications

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Dust in the bright supernova remnant N49 in the LMC

Herschelimages of NGC 6720: H₂formation on dust grains

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Calibration and Performance of the ISO Long-Wavelength Spectrometer

Cited by 114 publications

References 4 publications

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Dust in the bright supernova remnant N49 in the LMC

Herschelimages of NGC 6720: H2formation on dust grains

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Herschelimages of NGC 6720: H₂formation on dust grains