The Herschel–SPIRE instrument and its capabilities for extragalactic astronomy

Griffin, M. J.; Abergel, A.; André, P.; Baluteau, Jean-Paul; Bock, J. J.; Franceschini, A.; Gear, Walter Kieran; Glenn, J.; Griffin, Douglas; King, K. J.; Lellouch, E.; Madden, S.; Naylor, David; Oliver, Seb; Olofsson, G.; Page, M. J.; Pérez-Fournón, I.; Rowan-Robinson, M.; Saraceno, P.; Sawyer, Eric; Swinyard, Bruce; Vigroux, L.; Wright, Gillian

doi:10.1016/j.asr.2007.03.032

Cited by 29 publications

(26 citation statements)

References 16 publications

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“…Unfortunately, not many galaxies have detailed observations of the FIR/submm beyond the thermal peak. However, the advent of the SPIRE instrument aboard the Herschel satellite (Griffin et al 2007), in conjunction with the new ground-based submm facilities, will soon permit a more detailed study of this spectral range, necessary for constraining the bulk of dust mass.…”

Section: Discussionmentioning

confidence: 99%

“…10, I show the major axis surface brightness profiles of dust emission for the two disks and the clumpy models seen edge-on. Images have been smoothed with a PSF of FWHM = 16 , a resolution similar to what can be achieved, currently or in the next few years, at 70 μm using MIPS aboard the satellite Spitzer (Rieke et al 2004), at 250 μm using SPIRE aboard the satellite Herschel (Griffin et al 2007) and at 850 μm using the submm cameras SCUBA2 (Holland et al 2006) and LABOCA (Kreysa et al 2003). To these, I have added a profile at about 8 μm, centered on a large PAH feature.…”

Section: Attenuation Vs Inclination and Imagesmentioning

confidence: 99%

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Dust extinction and emission in a clumpy galactic disk

Bianchi¹

2008

A&A

116

201

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Aims. I present the Monte Carlo radiative transfer code TRADING (Transfer of RAdiation through Dust In Galaxies). The code selfconsistently computes the extinction of radiation in a dusty medium (including absorption and scattering) and the dust emission. Methods. A binary-tree adaptive grid is used for the description of the dust distribution. Dust radiation is computed at thermal equilibrium or under stochastic heating conditions, for a distribution of grains of different radii and materials. The code is applied to the case of a clumpy galactic disk, including both diffuse dust and a distribution of spherical clouds modelled on the GMCs of local galaxies. Diffuse and localised sources of starlight are used, with independent spectra. Results. A model is provided for the edge-on galaxy NGC 891. The SED of the galaxy from the UV to the submm/mm range can be well reproduced by a bulge/disk configuration of old stars together with an extended dust disk, as suggested by the analysis of optical/near-infrared images; a clumpy dust distribution of the same mass as the diffuse dust disk, together with a UV emitting component, half of which is in the form of a diffuse disk and half in sources embedded in clouds. In total, it is found that about 35% of the bolometric radiation is absorbed (and emitted) by dust; that absorption of starlight from the old population contributes to about 60% of the dust emission. A significant component of the dust emission from clouds is due to absorption of diffuse radiation. Radial profiles of dust emission in a clumpy disk are almost independent of the wavelength, with the exception of the wavelength range on the Wien side of the thermal equilibrium peak.

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Section: Discussionmentioning

confidence: 99%

Section: Attenuation Vs Inclination and Imagesmentioning

confidence: 99%

Dust extinction and emission in a clumpy galactic disk

Bianchi¹

2008

A&A

116

201

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“…The large systematic programme of cosmological surveys planned with Herschel over the whole far-IR and sub-mm spectral region (e.g. Griffin et al 2007Griffin et al , 2010 will soon both resolve the CIRB background into its individual sources and, in combination with pre-existing optical and Spitzer data over the survey areas, allow us to extensively sample the multi-wavelength luminosity functions. X-ray and radio data will offer additional diagnostic tools to disentangle the contributions of the two energy production mechanisms.…”

Section: Constraining the History Of Star Formation And Agn Accretionmentioning

confidence: 99%

Galaxy evolution from deep multi-wavelength infrared surveys: a prelude toHerschel

Franceschini

Rodighiero

Vaccari

et al. 2010

A&A

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Context. Studies of the generation and assembly of stellar populations in galaxies largely benefit from far-IR observations, considering that the IR flux is a close prior to the rate of star formation (the bulk of which happens in dust-obscured environments). At the same time, major episodes of nuclear AGN accretion are also dust-obscured and visible in the IR. Aims. At the end of the Spitzer cryogenic mission and the onset of the Herschel era, we review our current knowledge of galaxy evolution at IR wavelengths, and model it to achieve as far as a complete view of the evolution of cosmic sources. We also develop new tools for the analysis of background fluctuations to constrain source counts in regimes of high confusion, as it happens for the Herschel sub-mm surveys. Methods. We analysed a wide variety of new data on galaxy evolution and high-redshift source populations from Spitzer cosmological surveys, and confront them with complementary data from mm ground-based observations and constraints from the far-IR diffuse radiation, as well as preliminary results from Herschel surveys. Results. These data confirm earlier indications about a very rapid increase in galaxy volume emissivity with redshift up to z 1 [ρ(z) ∝ (1 + z) 4 ], the fastest evolution rate observed for galaxies at any wavelengths. The observed Spitzer counts require a combination of fast evolution for the dominant population and a bumpy spectrum with substantial PAH emission at z ∼ 1 to 2. Number counts at long wavelengths (70 through 1100 μm) confirm these results. All the present data require that the fast observed evolution from z = 0 to 1 flattens around redshift 1 and then keeps approximately constant up to z 2.5 at least. Our estimated redshift-dependent bolometric comoving energy density keeps lower at z > ∼ 1.5 than some previously published results based on either large extinction corrections, or large spectral extrapolations.Conclusions. The present-day IR/sub-mm data provide evidence of a distinct population of very luminous galaxies becoming dominant at z > 1. Their cosmological evolution, peaking around z 2, shows a faster decay with cosmic time than lower luminosity systems, whose maximal activity is set around z 1, then supporting an earlier phase of formation for the most luminous and massive galaxies. From a comparison of our results on the comoving IR emissivity with recent estimates of the redshift-dependent stellar mass functions of galaxies, we find that the two agree well with each other if we assume standard recipes for star formation (a universal Salpeter IMF) and standard fractions (∼20−30%) for the contribution of obscured AGN accretion. Systematic exploitation of the forthcoming Herschel survey data will be important for confirming all this.

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“…Silicon nitride thermal isolation was originally developed for ground-based and balloon-borne mm-wave instruments (SuZIE, BOOMERANG, BOLOCAM, BLAST), and later adapted for use in the PLANCK-HFI [1] and HERSCHEL-SPIRE [2] instruments, as well as in all of the current ground-based and balloon-borne instruments such as SCUBA2 and CLOVER. The rapid development of TESs over the last decade TES technology has increased its technology readiness level, and has paved the way for use on future space missions such as B-Pol, SPICA, and FIRI.…”

Section: Introductionmentioning

confidence: 99%

Optical requirements and modeling of coupling devices for future far-infrared space missions

et al. 2010

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The next generation of space missions targeting far-infrared bands will require large-format arrays of extremely lownoise detectors. The development of Transition Edge Sensors (TES) array technology seems to be a viable solution for future mm-wave to Far-Infrared (FIR) space applications where low noise and high sensitivity is required. In this paper we concentrate on a key element for a high sensitivity TES detector array, that of the optical coupling between the incoming electromagnetic field and the phonon system of the suspended membrane. An intermediate solution between free space coupling and a single moded horn is where over-moded light pipes are used to concentrate energy onto multimoded absorbers. We present a comparison of modeling techniques to analyze the optical efficiency of such light pipes and their interaction with the front end optics and detector cavity.

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The Herschel–SPIRE instrument and its capabilities for extragalactic astronomy

Cited by 29 publications

References 16 publications

Dust extinction and emission in a clumpy galactic disk

Dust extinction and emission in a clumpy galactic disk

Galaxy evolution from deep multi-wavelength infrared surveys: a prelude toHerschel

Optical requirements and modeling of coupling devices for future far-infrared space missions

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