IRAS observations of active galaxies

The IRAS survey gives an unbiased view of the infrared properties of the active galaxies. Seyfert galaxies occupy much the same area in color-color plots as to normal infrared bright galaxies, but extend the range towards flatter 60 to 25 mm slopes. Statistically the Seyfert 1 galaxies can be distinguished from the Seyfert 2 galaxies, lying predominantly closer to the area with constant slopes between 25 and 200 mm. The infrared measurements of the Seyfert galaxies cannot distinguish between the emission mechanisms in these objects although they agree with the currently popular ideas; they do provide a measure of the total luminosity of the Seyferts. The quasar's position in the color-color diagrams continue the trend of the Seyferts. The quasar 3C48 is shown to be exceptional among the radio loud quasars in that it has a high infrared luminosity which dominates the power output of the quasar and is most likely associated with the underlying host galaxy

SWS observations of IR emission features towards compact HII regions

We present ISO Short Wavelength Spectrometer (SWS) grating spectra of six compact HII regions. In addition to strong emission lines from atomic species these spectra display infrared bands attributed to Polycyclic Aromatic Hydrocarbons (PAHs). The continuous spectral coverage of the present observations and the high spectral resolution allow to describe the detailed structure of the emission bands: the 7.7μm band is composed of two bands at 7.6 and 7.8μm, the 6.2 μm band has a long wavelength extension, there is a plateau of emission between 6 and 7μm and a new feature is reported at 11.0μm in addition to the well-known 11.2μm band. These observations also reveal large variations in the relative intensities of the dust bands, in particular between the 7.7 and 8.6μm bands. In one extreme case, the 8.6μm band is stronger than the 7.7μm band. These observations are compared to a mixed population of ionized PAHs, using new laboratory measurements

Extragalactic Results from the Infrared Space Observatory

More than a decade ago the IRAS satellite opened the realm of external galaxies for studies in the 10 to 100 micron band and discovered emission from tens of thousands of normal and active galaxies. With the 1995-1998 mission of the Infrared Space Observatory the next major steps in extragalactic infrared astronomy became possible: detailed imaging, spectroscopy and spectro-photometry of many galaxies detected by IRAS, as well as deep surveys in the mid- and far- IR. The spectroscopic data reveal a wealth of detail about the nature of the energy source(s) and about the physical conditions in galaxies. ISO's surveys for the first time explore the infrared emission of distant, high-redshift galaxies. ISO's main theme in extragalactic astronomy is the role of star formation in the activity and evolution of galaxies.Comment: 106 pages, including 17 figures. Ann.Rev.Astron.Astrophys. (in press), a gzip'd pdf file (667kB) is also available at http://www.mpe.mpg.de/www_ir/preprint/annrev2000.pdf.g

ISO spectroscopy of gas and dust: from molecular clouds to protoplanetary disks

Observations of interstellar gas-phase and solid-state species in the 2.4-200 micron range obtained with the spectrometers on board the Infrared Space Observatory are reviewed. Lines and bands due to ices, polycyclic aromatic hydrocarbons, silicates and gas-phase atoms and molecules (in particular H2, CO, H2O, OH and CO2) are summarized and their diagnostic capabilities illustrated. The results are discussed in the context of the physical and chemical evolution of star-forming regions, including photon-dominated regions, shocks, protostellar envelopes and disks around young stars.Comment: 56 pages, 17 figures. To appear in Ann. Rev. Astron. Astrophys. 2004. Higher resolution version posted at http://www.strw.leidenuniv.nl/~ewine/araa04.pd

An ISO Long Wavelength Spectrometer detection of CH in NGC 7027 and an HeH + upper limit

We have detected an emission line at 149.18 ± 0.06 Ωm in the ISO Long Wavelength Spectrometer (LWS) grating spectrum of the planetary nebula NGC 7027. This Une coincides in wavelength with both the HeH+ J=1-0 fundamental pure rotational line at 149.14 urn and the CH 2Π3/2 (F2) J=3/2-2Πl/2 (F2) 7= 1/2 fundamental pure rotational lines at 149.09 and 149.39 μm. Another feature of similar strength at 180.7 urn is well-fitted by the CH doublet 2Π1/2 (F1) J=5/2-3/2 at 180.48 and 180.93 μm. We therefore attribute both the 149.18- and 180.7-um lines to CH, the first evidence of this molecule in NGC 7027 and the first detection anywhere of the far-infrared lines of CH in emission. We estimate a CH/CO abundance ratio of ∼ 0.06 and a CH/CH+ ratio of ∼0.2, the latter being more than an order of magnitude lower than predicted for photodissociation regions. The contribution from the HeH+ J=1−0 line to the 149.18-μm feature is at least a factor of three lower than the predictions of Cecchi-Pestellini & Dalgarno (1993)

The ISO LWS grating spectrum of NGC 7027

We present a high signal-to-noise ISO Long Wavelength Spectrometer (LWS) grating spectrum of the planetary nebula NGC 7027 from 43-194μm. In total 40 emission lines have been detected, with 30 identified. From the ionized region, we observe fine-structure lines from [N II], [N III] and [O III]. The [O I] and [C II] fine-structure lines from the photodissociation region are the strongest features observed in this spectral region. Amongst the molecular lines, 11 pure rotation CO lines from J=14-13 up to J=24-23 have been detected. The most striking result, however, is the detection in this carbon-rich nebula of the o-H_2_O 179.53μm and the OH 119.3μm fundamental lines. Astrophysical implications are briefly discussed

Calibration and performance of the ISO Long-Wavelength Spectrometer

The wavelength and flux calibration, and the in-orbit performance of the Infrared Space Observatory Long-Wavelength Spectrometer (LWS) are described. The LWS calibration is mostly complete and the instrument's performance in orbit is largely as expected before launch. The effects of ionising radiation on the detectors, and the techniques used to minimise them are outlined. The overall sensitivity figures achieved in practice are summarised. The standard processing of LWS data is described

Emerging variants of canine enteric coronavirus associated with seasonal outbreaks of severe canine gastroenteric disease

Canine enteric coronavirus (CECoV) variants have an emerging role in severe outbreaks of canine gastroenteritis. Here we used syndromic health data from a sentinel network of UK veterinary practices to identify an outbreak of severe canine gastroenteritis. Affected dogs frequently presented with vomiting, diarrhoea and inappetence. Data from sentinel diagnostic laboratories showed similar seasonal increases in CECoV diagnosis. Membrane glycoprotein (M) gene sequence analysis implied wide geographical circulation of a new CECoV variant. Whole genome sequencing suggested the main circulating 2022 variant was most closely related to one previously identified in 2020 with additional spike gene recombination; all variants were unrelated to CECoV-like viruses recently associated with human respiratory disease. Identifying factors that drive population-level evolution, and its implications for host protection and virulence, will be important to understand the emerging role of CECoV variants in canine and human health, and may act as a model for coronavirus population adaptation more widely

The ISO long-wavelength spectrometer

The Long-Wavelength Spectrometer (LWS) is one of two complementary spectrometers aboard the European Space Agency's Infrared Space Observatory (ISO) (Kessler et al., 1996A&A...315L..49D). It operates over the wavelength range 43-196.9μm at either medium (about 150 to 200) or high (6800 to 9700) spectral resolving power. This Letter describes the instrument and its modes of operation; a companion paper (Swinyard et al, 1996) describes its performance and calibration