Correcting the extended-source calibration for the Herschel-SPIRE Fourier-transform spectrometer

Valtchanov, I.; Hopwood, R.; Bendo, G. J.; Benson, Chris S.; Conversi, L.; Fulton, T.; Griffin, Matthew Joseph; Joubaud, T.; Lim, T.; Lu, N.; Marchili, N.; Makiwa, G.; Meyer, Romain A.; Naylor, David; North, C.; Παπαγεωργίου, Ανδρέας; Pearson, Chris; Polehampton, E. T.; Scott, Jeremy P.; Schulz, B.; Spencer, L. D.; Wiel, M. H. D. van der; Wu, R.

doi:10.1093/mnras/stx3178

Cited by 10 publications

(10 citation statements)

References 35 publications

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“…The SPIRE-FTS data were downloaded from the Herschel Science Archive, processed using HIPE v14.1, with SPIRE calibration files spire_cal_14_3. The FTS extended source calibration (Swinyard et al 2014) was used, and in HIPE v14.1, this includes the updates described in Valtchanov et al (2018) to align the absolute brightness level to match the SPIRE photometer.…”

Section: Spirementioning

confidence: 99%

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Globules and pillars in Cygnus X

Schneider

Röllig

Polehampton

et al. 2021

A&A

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IRAS 20319+3958 in Cygnus X South is a rare example of a free-floating globule (mass ~240 M⊙, length ~1.5 pc) with an internal H II region created by the stellar feedback of embedded intermediate-mass stars, in particular, one Herbig Be star. In Schneider et al. 2012, (A&A, 542, L18) and Djupvik et al. 2017, (A&A, 599, A37), we proposed that the emission of the far-infrared (FIR) lines of [C II] at 158 μm and [O I] at 145 μm in the globule head are mostly due to an internal photodissociation region (PDR). Here, we present a Herschel/HIFI [C II] 158 μm map of the whole globule and a large set of other FIR lines (mid-to high-J CO lines observed with Herschel/PACS and SPIRE, the [O I] 63 μm line and the 12CO 16→15 line observed with upGREAT on SOFIA), covering the globule head and partly a position in the tail. The [C II] map revealed that the whole globule is probably rotating. Highly collimated, high-velocity [C II] emission is detected close to the Herbig Be star. We performed a PDR analysis using the KOSMA-τ PDR code for one position in the head and one in the tail. The observed FIR lines in the head can be reproduced with a two-component model: an extended, non-clumpy outer PDR shell and a clumpy, dense, and thin inner PDR layer, representing the interface between the H II region cavity and the external PDR. The modelled internal UV field of ~2500 G° is similar to what we obtained from the Herschel FIR fluxes, but lower than what we estimated from the census of the embedded stars. External illumination from the ~30 pc distant Cyg OB2 cluster, producing an UV field of ~150–600 G° as an upper limit, is responsible for most of the [C II] emission. For the tail, we modelled the emission with a non-clumpy component, exposed to a UV-field of around 140 G°.

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Section: Spirementioning

confidence: 99%

“…Our data include the latest corrections to match the FTS extended calibration to the SPIRE Photometer (Valtchanov et al 2018).…”

Section: Upgreat: [O I] 63 µM and Co 16→15mentioning

confidence: 99%

Globules and pillars in Cygnus X

Schneider

Röllig

Polehampton

et al. 2021

A&A

View full text Add to dashboard Cite

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“…The archival data have been reprocessed through HIPE 15.0.1 using the latest available SPIRE calibration (version 14.3) and the flux calibration for extended emission. It is important to notice that this version of the SPIRE calibration corrects for an important error in extended source flux calibration discovered by Valtchanov et al (2018). This error was corrected with version 14.2 of the SPIRE calibration in Nov 2015 and used in the developer version of HIPE 14 1 .…”

Section: Herschel/pacs Spectramentioning

confidence: 99%

[CII] map of the molecular ring and arms of the spiral galaxy NGC 7331

Sutter,

Fadda

2021

Preprint

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We present the [CII] 157.7 µm map of galaxy NGC 7331 obtained with FIFI-LS on SOFIA. This map extends an existent Herschel/PACS observation of the central strip of the galaxy to encompass the entire molecular ring and much of the disk, including multiple spiral arms with intense far-IR emission. We also present Herschel archival data of the [NII] 205 µm line which covers a substantial part of the [CII] SOFIA observations and allows us to estimate the neutral fraction of the [CII] emission along the ring and disk of the galaxy. We find that the neutral fraction rises with the distance from the center. In addition, by tracing the azimuthal variation of the neutral fraction, we are able to see how our observing perspective affects this measurement. The high inclination of NGC 7331 allows us to glimpse the internal walls of the molecular ring. There, young bright stars emit UV radiation causing more [CII] emission to be produced in the ionized gas. On the outer walls, opaque dust shrouds the rest of the ring, making the neutral medium the dominant source of [CII] emission. Through spatial analysis comparing the [CII] emission to tracers of gas heating, we are able to investigate how the photoelectric heating efficiency varies throughout NGC 7331 and extend global measurements of the [CII] deficit to local environments. Since the origin of [CII] emission has typically been studied in face-on galaxies, our results shed a new light on the interpretation of [CII] emission especially when studying distant galaxies with unknown inclination.

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“…The SPIRE-FTS data were downloaded from the Herschel Science Archive, processed using HIPE v14.1, with SPIRE calibration files spire_cal_14_3. The FTS extended source calibration (Swinyard et al 2014) was used, and in HIPE v14.1, this includes the updates described in (Valtchanov et al 2018) to align the absolute brightness level to match the SPIRE photometer.…”

Section: Spirementioning

confidence: 99%

Globules and pillars in Cygnus X III. Herschel and upGREAT/SOFIA far-infrared spectroscopy of the globule IRAS 20319+3958 inCygnus X

Schneider,

Roellig,

Polehampton

et al. 2021

Preprint

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IRAS 20319+3958 in Cygnus X South is a rare example of a free-floating globule (mass ∼240 M , length ∼1.5 pc) with an internal H II region created by the stellar feedback of embedded intermediate-mass stars, in particular, one Herbig Be star. In Schneider et al. (2012) andDjupvik et al. (2017), we proposed that the emission of the far-infrared (FIR) lines of [C II] at 158 µm and [O I] at 145 µm in the globule head are mostly due to an internal photodissociation region (PDR). Here, we present a Herschel/HIFI [C II] 158 µm map of the whole globule and a large set of other FIR lines (mid-to high-J CO lines observed with Herschel/PACS and SPIRE, the [O I] 63 µm line and the 12 CO 16→15 line observed with upGREAT on SOFIA), covering the globule head and partly a position in the tail. The [C II] map revealed that the whole globule is probably rotating. Highly collimated, high-velocity [C II] emission is detected close to the Herbig Be star. We performed a PDR analysis using the KOSMA-τ PDR code for one position in the head and one in the tail. The observed FIR lines in the head can be reproduced with a two-component model: an extended, non-clumpy outer PDR shell and a clumpy, dense, and thin inner PDR layer, representing the interface between the H II region cavity and the external PDR. The modelled internal UV field of ∼2500 G • is similar to what we obtained from the Herschel FIR fluxes, but lower than what we estimated from the census of the embedded stars. External illumination from the ∼30 pc distant Cyg OB2 cluster, producing an UV field of ∼150-600 G • as an upper limit, is responsible for most of the [C II] emission. For the tail, we modelled the emission with a non-clumpy component, exposed to a UV-field of around 140 G • .

show abstract

Correcting the extended-source calibration for the Herschel-SPIRE Fourier-transform spectrometer

Cited by 10 publications

References 35 publications

Globules and pillars in Cygnus X

Globules and pillars in Cygnus X

[CII] map of the molecular ring and arms of the spiral galaxy NGC 7331

Globules and pillars in Cygnus X III. Herschel and upGREAT/SOFIA far-infrared spectroscopy of the globule IRAS 20319+3958 inCygnus X

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