Infrared spectroscopy is the best astronomical tool for studying the composition of cosmic dust. Thanks to the Herschel satellite, dust properties from the FIR to mm wavelength range will be sampled in different astrophysical environments. In the laboratory, the study of the temperature and structural dependence of FIR absorption of cosmic dust analogs including agglomeration is essential to interpret observational spectra. For crystalline materials, FIR single phonon bands are temperature dependent due to the anharmonicity of the vibrational potentials. This strong temperature dependence of the FIR bands’ positions can be used as a thermometer of the dust temperature. In amorphous material, the FIR absorption is dominated by disorder-induced single phonon processes and in the submillimeter and millimeter range by highly temperature-dependent low energy processes, e.g. tunneling transitions in two-level systems. The effect of these processes on the FIR absorptivity in amorphous silicates will be demonstrated.

We present an overview of SPICA, the Space Infrared Telescope for Cosmology and Astrophysics, a world-class space observatory optimized for mid- and far-IR astronomy (from 5 to  ~210 μm) with a cryogenically cooled  ~3.2 m telescope (<6 K). Its high spatial resolution and unprecedented sensitivity in both photometry and spectroscopy modes will enable us to address a number of key problems in astronomy. SPICA’s large, cold aperture will provide a two order of magnitude sensitivity advantage over current far–IR facilities (λ > 30μm wavelength). In the present design, SPICA will carry mid-IR camera, spectrometers and coronagraph (by JAXA institutes) and a far-IR imager FTS-spectrometer, SAFARI (~34–210 μm, provided by an European/Canadian consortium lead by SRON). Complementary instruments such as a far-IR/submm spectrometer (proposed by NASA) are also being discussed. SPICA will be the only space observatory of its era to bridge the far–IR wavelength gap between JWST and ALMA, and carry out unique science not achievable at visible or submm wavelengths. In this contribution we summarize some of the scientific advances that will be made possible by the large increase in sensitivity compared to previous infrared space missions.

Polarimetry at far-infrared wavelengths is a key tool for studying physical processes on size scales ranging from interstellar dust grains to entire galaxies. A multi-wavelength continuum polarimeter at these wavelengths will allow studies of thermal dust polarization in an effort to constrain the grains’ physical properties and test grain alignment theory. High spatial resolution (5–30 arcsec) and sensitive observations will measure the influence of magnetic fields on infrared cirrus clouds, the envelopes and disks of YSOs, outflows from both low- and high-mass star forming regions, and the relative strength of magnetic, gravitational, and turbulent effects in star- and cloud-formation.

The Echelon-cross-Echelle Spectrograph (EXES), one of the first generation instruments for the Statospheric Observatory for Infrared Astronomy (SOFIA) will provide a unique tool for examining the ISM and star formation. The EXES high spectral resolution mode, R  ≤  120 000 from 4.5 μm to 28.3 μm, is designed for line observations of gas-phase molecules. The improved atmospheric transmission guaranteed by SOFIA will make observations of molecules such as H2O and CH4 fairly routine. EXES will also have medium and low resolution modes to enable a wide range of science projects. EXES is a PI instrument open for collaborative proposals following the model of the successful TEXES instrument (Lacy et al. 2002). It is currently scheduled for first science flights on SOFIA in 2013.

We present an update on the performance of our 2 mm bolometer camera GISMO (the Goddard IRAM 2 Millimeter Observer), which is used for astronomical observations at the IRAM 30 m Telescope. The camera is optimized to efficiently observe dusty high-redshift galaxies. GISMO uses a monolithic 8 by 16 Backshort Under Grid (BUG) array with superconducting Transition Edge Sensors (TES). It serves as a testbed for our close-packed superconducting bolometer technologies and guides us in optimizing the design of future fast, low background bolometer cameras. Illustrated by astronomical observations we obtained recently, we demonstrate the scientific potential of the camera, highlighted by the detection of two high redshift galaxies.

We evaluate radiation pressure from starlight on dust as a feedback mechanism instar-forming galaxies by comparing the luminosity and flux of star-forming systems to thedust Eddington limit. The linearLFIR–\hbox{$L_{\rm HCN}^\prime$}${\mathit{L}}_{\mathrm{HCN}}^{\mathrm{\prime }}$ correlationprovides evidence that galaxies may be regulated by radiation pressure feedback. We showthat star-forming galaxies approach but do not dramatically exceed Eddington, but manysystems are significantly below Eddington, perhaps due to the “intermittency” of starformation. Better constraints on the dust-to-gas ratio and the CO- andHCN-to-H2 conversion factors are needed to make a definitive assessment ofradiation pressure as a feedback mechanism.

We use the DustEM model coupled with a radiative transfer code to fit the Herschel and Spitzer emission of the Orion Bar. The thermal dust emission at the 250-μm peak position is well reproduced but we overestimate the stochastically heated grain emission. The dust model parameters are checked with the Meudon PDR code and are consistent with the spectroscopic data from the SPIRE FTS.

New images of the interstellar medium provided by Herschel and Planck bring spectacular evidence of the intricate and filamentary structure of the interstellar medium, betraying its turbulent nature. Although turbulence is a subject of interest in astronomy, little is know about the origin of turbulence in the interstellar medium. We suggest that part of the turbulence in the Orion molecular cloud be due to the decay of the Kelvin-Helmholtz instability.

Observations of HDO are an important complement for studies of water, because they givestrong constraints on the formation processes – grain surfaces versusenergetic process in the gas phase, e.g. in shocks. The HIFIobservations of multiple transitions of HDO in Sgr B2(M) presented here allow thedetermination of the HDO abundance throughout the envelope, which has not been possiblebefore with ground-based observations only. For more details, see Comito et al.(2010).

Here we present the results of a 3 mm survey of 23 galaxies, obtained with the EMIRreceiver at the IRAM 30 m telescope. Emission of the main molecular species is comparedwith existing chemical models, in order to find and test molecular signatures of galaxyevolution and to compare them to IR evolutionary tracers.

In the Magellanic Clouds, the [CII]/CO and the [CII]/FIR ratios are much higher than seen in Milky Way star-forming regions. The enhanced relative strength of the [CII] line reflects the physical environment characterised by the low metallicities, dust abundances, and PAH abundances of the LMC, and especially the SMC.

We have analyzed the distributions of CO and temperature in a large suite of simulatedmolecular clouds, in order to help us understand how to interpret CO line emission fromreal molecular clouds. We find that most of the CO is located at densities over103cm-3 where the temperature is roughly 10–20 K independently ofthe mean density, metallicity and UV field strength. Although, most of the volume is inwarmer and thinner regions where CO abundance is small. On that account, CO observationsalone give a misleading view of the physical conditions in the clouds.

Observations of CH+, J = 1 − 0 and 2 − 1 near 0.835 and 1.67THz with Herschel/HIFI and of 13CH+, J = 1 − 0 near0.830 THz with APEX revealed their rest frequencies to be higher than the accepted valuesby 21 and 30 km s-1, respectively. Very recent laboratory measurements of theJ = 1 − 0 transition frequencies of CH+,13CH+ and CD+ and fits to these as well as electronicspectral data resolved the descrepancies. The laboratory spectroscopic situation will bereviewed for selected cationic light hydride species.

We report the analysis of the mid-infrared spectral maps observed by Spitzer/IRS toward star-forming regions where the Herschel key program WADI has observed / will observe with HIFI and PACS. The IRS spectra are fitted using 4 components of small grains: PAH0, PAH+, PAHx, and evaporating VSG, and the spatial distributions of these components are derived.

We present a full spectral view of Arp 220 from 450 GHz to 1500 GHz usingHerschel SPIRE. The non-LTE modeling of mid-J to high-J CO linessuggests surprisingly warm molecular gas between 500 and 1500 K, the mass of which isabout 1% of the cold gas mass.

Spectral surveys provide the only way to determine the full molecular inventory of a source and hence to build a comprehensive view of the state of the molecular gas and its role in the star formation process. Systematic studies have opened the possibility of using chemistry as a diagnostic tool for star burst and AGN activities in the highly obscured galactic nuclear regions.

We present HIFI observations of [CII] and high-J transitions of CO and HCO+ atpositions in S140 and DR21. We use a clumpy PDR model to model and interpret the observedline intensities. The emission from both massive star forming regions can be reproduced byassuming a clumpy, 2-component PDR scenario.

Hot molecular cores are a short-lived phase of massive star formation: the massive stars have heated up the dense molecular gas in which they are deeply embedded, but have not yet ionized and disrupted it. Information on their structure (density, temperature, velocity, molecular abundances) is needed both for research on massive star formation and for astrochemistry. We constrain their structure by radiative transfer modeling of a variety of molecular lines, including from highly excited states, using APEX and Herschel/HIFI. To spatially resolve the hot molecular gas, we performed VLA and SMA observations. In this article, we summarize some to the results.

The Rosette molecular cloud has a characteristic morphology, where the central OB cluster NGC 2244 has blown a circular-shaped cavity into the cloud and the expanding HII-region now interacts with the cloud. We use continuum data obtained with the PACS (70 and 160 μm) and SPIRE instruments (250, 350, 500 μm) of the Herschel telescope to investigate the spatial distribution of cold and warm gas and to locate all star-forming sites in Rosette. We detected a clear negative temperature gradient and a positive density gradient (running from the HII-region/molecular cloud interface into the cloud), and an age-sequence (from more evolved to younger) with increasing distance to the cluster NGC 2244. The existence of such temperature and density gradients and the observed age-sequence imply that star formation in Rosette may indeed be influenced by the radiative impact of the central NGC 2244 cluster.