We compute the cosmic stellar, dust, and neutral gas mass history at 0 < z less than or similar to 3 using PROSPECT spectral energy distribution modelling of approximate to 800 000 galaxies in the Galaxy and Mass Assembly survey and the Deep Extragalactic VIsible Legacy Survey. The cosmic dust mass history broadly follows the shape of the cosmic star formation history; however, the decline is slower, suggestive of a slowing rate of dust growth and destruction as the star formation declines past its peak at z approximate to 2 . Neutral gas masses were estimated by scaling the dust masses by the metallicity-dependent dust-to-gas ratio. The neutral gas mass density as traced by the dust is an average of approximate to 0 . 7 dex lower than that measured from 21 cm experiments, most likely due to differences in the spatial scales inhabited by dust and HI. Folding in measurements of the supermassive black hole (SMBH) mass density obtained previously with similar data and methods, we present a self-consistent census of the baryons confined to galaxies. Stars, neutral gas, SMBHs, and dust contained within the optical radii of galaxies account for ti 5 per cent of the baryons. Most of the remaining ti 95 per cent of baryons must be ionized and dispersed throughout the interstellar, circumgalactic, and intergalactic media within, around, and between galaxies.

Despite the implied presence of dust through reddened UV emission in high-redshift galaxies, no dust emission has been detected in the (sub)millimetre regime beyond z > 8 . 3. This study combines around 200 h of Atacama Large Millimetre/submillimetre Array (ALMA) and Northern Extended Millimetre Array (NOEMA) observations on 10 z > 8 galaxies, revealing no significant dust emission down to a 1 Q of 2.0, 2.0, and 1 . 5 at rest-frame 158, 88 and across all the data, This constrains average dust masses to be below < 10( 5 )M(circle star) at 3 sigma and dust-to-stellar mass ratios to be below 3 . 7 x 10(-4 )(assuming T-dust = 50 K and beta(dust )= 2 . 0). Binning by redshift (8 < z < 9 . 5 and 9 . 5 < z < 15), UV-continuum slope (eUV less than or greater than -2), and stellar mass (log(10) M-*/ M-circle star less than or greater than 9) yields similarly stringent constraints. Combined with other studies, these results are consistent with inefficient dust build-up in the z > 8 Universe, likely due to inefficient supernova production, limited interstellar grain growth and/or ejection by outflows. We provide data and tools online to facilitate community-wide high-redshift dust searches.

We have carried out a stacking analysis with the COSMOS-Web catalogue on one of the deepest ever SCUBA-2 images at 850-mu m, allowing us to estimate the mean submillimetre flux density for samples of galaxies split by stellar mass and morphological class over the redshift range 0 < z <12 . For all morphological classes, the mean star formation rate estimated from the dust emission increases with redshift, reaching a value for the most massive galaxies (M-& lowast;similar or equal to 10(11)M(circle dot)) of similar or equal to 80 M(circle dot)yr(-1)at 2< z< 4.5 In this redshift range, the mean star formation rate for these galaxies falls along the Hubble sequence from similar or equal to 280 M(circle dot )yr(-1 )for irregular galaxies at one end to similar or equal to M(circle dot )yr(-1) for spheroids at the other end, which shows that quenching was already happening shortly after the emergence of the Hubble sequence. We also show that the transformation of 'submillimetre galaxies' can reproduce the growth in number density of massive bulge-dominated and spheroidal galaxies over the redshift range 1.5 < z < 4. As a side project, we have used our stacking results to determine the relationship between the mean density of dust and redshift in the range 0 < z < 12. We show that a chemical evolution model based on the 'star formation history' of the universe, with a gas outflow rate equal to the star formation rate, can explain the monotonic rise with redshift in the dust-to-stellar mass ratio and reproduce the relationship between mean dust density and redshift remarkably accurately.

The Mexico-UK Submillimeter Camera for AsTronomy (MUSCAT) is a continuum camera in the 1.1-mm band for the Large Millimeter Telescope (LMT), with 1458 lumped-element kinetic inductance detectors distributed across six arrays. Installed on the telescope at the end of 2021, we present the characterization of the detector beams of four of the six arrays based on the beam map observations of bright point sources developed during the first commissioning campaign between February and June 2022. With all the observations, we estimate the average positions of each detector with an average error in azimuth of less than 0.70 arcsec and less than 1.05 arcsec in elevation. From the positions, we created the coadded maps of all the detectors, from which we selected only eight observations to calculate the mean beam width of MUSCAT-LMT, of 6.32 +/- 0.36 arcsec x5.78 +/- 0.19 arcsec. By stacking the maps, we identify the sidelobes with three main structures whose amplitudes are similar to 3% with respect to the main beam.

We estimate how the mean density of dust in the Universe varies with redshift, using submillimetre continuum observations and a method designed to minimize the effect of dust temperature. We have used the Herschel Astrophysical Terahertz Large Area Survey (Herschel-ATLAS) to show that the median temperature of dust in galaxies is similar or equal to 22 K and does not vary significantly with redshift out to z = 1. With this as our estimate of the mass-weighted dust temperature, we have used an 850-um survey of the field of the Cosmological Evolution Survey (COSMOS) to estimate the mean density of dust in 10 redshift bins over the range 0 < z < 5.5. We find that the mean density of dust increased by a factor of similar or equal to 10 from z = 5 to z = 2, declined slightly to z = 1, and then steeply to the present day. The relationship between the mean density of dust and redshift is similar to the relationship between the mean star formation rate and redshift, although the increase for the former is steeper from z = 5 to z = 2. We have also used the submillimetre measurements to estimate the mean density of gas over the same redshift range. The values we estimate for the dust-traced gas are much lower and with a different redshift dependence than those for estimates of the mean density of atomic gas but similar to those for estimates of the mean density of the CO-traced gas. We find that the depletion time for the dust-traced gas in the Universe as a whole declines with redshift in the same way as seen for individual galaxies.

This paper forms part of the second major public data release of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). In this work, we describe the identification of optical and near-infrared counterparts to the submillimetre detected sources in the 177 deg(2) North Galactic Plane (NGP) field. We used the likelihood ratio method to identify counterparts in the Sloan Digital Sky Survey and in the United Kingdom InfraRed Telescope Imaging Deep Sky Survey within a search radius of 10 arcsec of the H-ATLAS sources with a 4 sigma detection at 250 mu m. We obtained reliable (R >= 0.8) optical counterparts with r < 22.4 for 42 429 H-ATLAS sources (37.8 per cent), with an estimated completeness of 71.7 per cent and a false identification rate of 4.7 per cent. We also identified counterparts in the near-infrared using deeper K-band data which covers a smaller similar to 25 deg(2). We found reliable nearinfrared counterparts to 61.8 per cent of the 250-mu m-selected sources within that area. We assessed the performance of the likelihood ratio method to identify optical and near-infrared counterparts taking into account the depth and area of both input catalogues. Using catalogues with the same surface density of objects in the overlapping similar to 25 deg(2) area, we obtained that the reliable fraction in the near-infrared (54.8 per cent) is significantly higher than in the optical (36.4 per cent). Finally, using deep radio data which covers a small region of the NGP field, we found that 80-90 per cent of our reliable identifications are correct.

In most studies of dust in galaxies, dust is only detected from its emission to approximately the optical radius of the galaxy. By combining the signal of 110 spiral galaxies observed as part of the Herschel Reference Survey, we are able to improve our sensitivity by an order of magnitude over that for a single object. Here we report the direct detection of dust from its emission that extends out to at least twice the optical radius. We find that the distribution of dust is consistent with an exponential at all radii with a gradient of similar to-1.7 dex R-25(-1). Our dust temperature declines linearly from similar to 25 K in the centre to 15 K at R-25 from where it remains constant out to similar to 2.0 R-25. The surface density of dust declines with radius at a similar rate to the surface density of stars but more slowly than the surface density of the star-formation rate. Studies based on dust extinction and reddening of high-redshift quasars have concluded that there are substantial amounts of dust in intergalactic space. By combining our results with the number counts and angular correlation function from the SDSS, we show that with Milky Way-type dust we can explain the reddening of the quasars by the dust within galactic discs alone. Given the uncertainties in the properties of any intergalactic dust, we cannot rule out its existence, but our results show that statistical investigations of the dust in galactic haloes that use the reddening of high-redshift objects must take account of the dust in galactic discs.

This paper is the second in a pair of articles presenting data release 1 (DR1) of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), the largest single open-time key project carried out with the Herschel Space Observatory. The H-ATLAS is a wide-area imaging survey carried out in five photometric bands at 100, 160, 250, 350 and 500$\mu$m covering a total area of 600deg$^2$. In this paper we describe the identification of optical counterparts to submillimetre sources in DR1, comprising an area of 161 deg$^2$ over three equatorial fields of roughly 12$^\circ$x4.5$^\circ$ centred at 9$^h$, 12$^h$ and 14.5$^h$ respectively. Of all the H-ATLAS fields, the equatorial regions benefit from the greatest overlap with current multi-wavelength surveys spanning ultraviolet (UV) to mid-infrared regimes, as well as extensive spectroscopic coverage. We use a likelihood-ratio technique to identify SDSS counterparts at r<22.4 for 250-$\mu$m-selected sources detected at $\geq$ 4$\sigma$ ($\approx$28mJy). We find `reliable' counterparts (reliability R$\geq$0.8) for 44,835 sources (39 per cent), with an estimated completeness of 73.0 per cent and contamination rate of 4.7 per cent. Using redshifts and multi-wavelength photometry from GAMA and other public catalogues, we show that H-ATLAS-selected galaxies at $z<0.5$ span a wide range of optical colours, total infrared (IR) luminosities, and IR/UV ratios, with no strong disposition towards mid-IR-classified AGN in comparison with optical selection. The data described herein, together with all maps and catalogues described in the companion paper (Valiante et al. 2016), are available from the H-ATLAS website at www.h-atlas.org.

The observations described here have been taken as part of the Herschel Multi-tiered Extragalactic Survey (HerMES; Oliver et al., 2012MNRAS.424.1614O) under the programme KPGT_soliver 1 whose main objective was to chart the formation and evolution of infrared galaxies throughout cosmic history, measuring the bolometric emission of infrared galaxies and their clustering properties. The catalogues extracted from these maps include over 1,200,000 entries representing over 340,000 galaxies. (11 data files).

The SCUBA Local Universe Galaxy Survey (SLUGS) is the first large systematic submm survey of the local Universe. Since our initial survey of a sample of 104 IRAS -selected galaxies ([1]) we have now completed a survey of a sample of 81 optically selected galaxies ([3]). Since SCUBA is sensitive to the 90% of dust too cold to radiate significantly in the IRAS bands our new sample represents the first unbiased submm survey of dust along the whole length of the Hubble sequence. We find little change in the properties of dust in galaxies along the Hubble sequence, and detected 6 out of 11 ellipticals. As in our earlier work on IRAS galaxies we find that the IRAS and submm fluxes are well fitted by a two-component dust model with dust emissivity index β=2. The major difference from our earlier work is the ratio of the mass of cold dust to the mass of warm dust, which is much higher for our optically selected galaxies, reaching values of ∼1000. Comparison of the results for the IRAS and optically selected samples shows that there is a population of galaxies containing a large proportion of cold dust that is unrepresented in the IRAS sample. We derive local submm luminosity and dust mass functions, both directly from our optically selected SLUGS sample, and by extrapolation from the IRAS PSCz survey using the method of Serjeant and Harrison ([2]), and find excellent agreement between the two. They are well fitted by Schechter functions except at the highest luminosities. We find that as a consequence of the omission of cold dusty galaxies from the IRAS sample the luminosity function presented in our earlier work is too low by a factor of 2, reducing the amount of cosmic evolution required between the low-z and high-z Universe.

We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio–mm–far-infrared (FIR) colours of 120 robustly detected 850 μm sources in the Lockman Hole East (LH) and Subaru XMM–Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radio–sub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy. The redshift distribution of sources derived from at least two photometric bands peaks at z≈ 2.4 and has a near-Gaussian distribution, with 50 per cent (interquartile range) of sources at z= 1.8–3.1 . We find a statistically significant difference between the measured redshift distributions in the two fields; the SXDF peaking at a slightly lower redshift (median z ≈ 2.2 ) than the LH (median z ≈ 2.7 ), which we attribute to the noise properties of the radio observations. We demonstrate, however, that there could also be field-to-field variations that are consistent with the measured differences in the redshift distributions and, hence, that the incomplete area observed by SHADES with SCUBA, despite being the largest sub-mm survey to date, may still be too small to fully characterize the bright sub-mm galaxy population. Finally, we present a brief comparison with the predicted, or assumed, redshift distributions of sub-mm galaxy formation and evolution models, and we derive the contribution of these SHADES sources and the general sub-mm galaxy population to the star formation rate density at different epochs.

The environmental properties of a sample of 31 hard X-ray selected active galactic nuclei (AGN) are investigated, from scales of 500 kpc down to 30 kpc, and are compared to a control sample of inactive galaxies. All the AGN lie in the redshift range 0.4 < z < 0.6. The accretion luminosity density of the Universe peaks close to this redshift range, and the AGN in the sample have X-ray luminosities close to the knee in the hard X-ray luminosity function, making them representative of the population that dominated this important phase of energy conversion. Using both the spatial clustering amplitude and near-neighbour counts, it is found that the AGN have environments that are indistinguishable from normal, inactive galaxies over the same redshift range and with similar optical properties. Typically, the environments are of subcluster richness, in contrast to similar studies of high-z quasars, which are often found in clusters with comparable richness to the Abell R≥ 0 clusters. It is suggested that minor mergers with low-mass companions are a likely candidate for the mechanism by which these modest luminosity AGN are fuelled.

It has been suggested by Dwek that iron needles could explain the submillimetre emission from the Cas A supernova remnant (SNR) with only a very small total mass. We investigate whether a similar model holds for the Kepler SNR, and find that its emission could indeed be explained by a dust mass of less than 10?2 M?, dependent on the axial ratio l/a of the needles – which we constrain to be less than 700. But the implied needle model for Kepler is inconsistent with that suggested for Cas A since either the needles would have to have a resistivity one or two orders of magnitude greater than those in Cas A or the electron density in Kepler's shocked plasma must be 40 times greater than suggested by X-ray observations. An additional problem with the needle model is that the implied thickness of the needles seems to be implausibly small, if the emission properties are calculated under the usual approximations.

The SCUBA HAlf Degree Extragalactic Survey (SHADES) is a major new blank-field extragalactic sub-mm survey currently underway at the James Clerk Maxwell telescope. Ultimately, SHADES aims to cover half a square degree at 450 and 850 µ m to a 4- σ depth of ≃ 8 mJy at 850 µ m. Two fields are being observed, the Subaru/XMM– Newton Deep Field (SXDF) (02 h 18 m − 05 ◦ ) and the Lockman Hole East (10 h 52 m +57 ◦ ). The survey has three main aims: i) to investigate the population of high-redshift sub-mm galaxies and the cosmic history of massive dust enshrouded star-formation activity, ii) to investigate the clustering properties of sub-mm–selected galaxies in order to determine whether these objects could be progenitors of present-day massive ellipticals, and iii) to investigate the fraction of sub-mm-selected sources that harbour active galactic nuclei. To achieve these aims requires that the sub-mm data be combined with co-spatial information spanning the radio–to–X-ray frequency range. Accordingly SHADES has been designed to benefit from ultra-deep radio imaging obtained with the VLA, deep mid-infrared observations from the Spitzer Space Telescope, sub-mm mapping by the Balloon-borne Large Area Sub-millimetre Telescope (BLAST), deep near-infrared imaging with the UK Infrared Telescope, deep optical imaging with the Subaru telescope, and deep X-ray observations with the XMM– Newton observatory. It is expected that the resulting extensive multi-wavelength dataset will provide complete photometric redshift information accurate to δz < ∼ 0 . 5, as well as detailed spectral energy distributions for the vast majority of the sub-mm-selected sources. In this paper, the first of a series on SHADES, we present an overview of the motivation for the survey, describe the SHADES survey strategy, provide a detailed description of the primary data analysis pipeline, and demonstrate the superiority of our adopted matched-filter source extraction technique over, for example, Emerson-II style methods. We also report on the progress of the survey. As of February 2004, 720 arcmin 2 had been mapped with SCUBA (about 40% of the anticipated final total area) to a median 1 σ depth of 2.2 mJy per beam at 850 µ m (25 mJy per beam at 450 µ m), and the source extraction routines give a source density of 650 ± 50 sources deg − 2 > 3 σ at 850 µ m. Although uncorrected for Eddington bias, this source density is more than suf-ficient for providing enough sources to answer the science goals of SHADES once half a square degree is observed. A refined re-analysis of the original 8-mJy survey Lockman hole data was carried out in order to evaluate the new data reduction pipeline. Of the 17 most secure sources in the original sample, 12 have been re-confirmed, including ten of the eleven for which radio identifications were previously secured.

We present the results of deep near-infrared spectroscopy of seven submillimetre-selected galaxies from the Submillimetre Common User Bolometer Array (SCUBA) 8-mJy Survey and Canada–UK Deep Submillimetre Survey (CUDSS). These galaxies were selected because they are too faint to be accessible to optical spectrographs on large telescopes. We obtain a spectroscopic redshift for one object, and likely redshifts for two more, based on a combination of marginal emission-line detections and the shape of the continuum. All three redshifts broadly agree with estimates from their radio/submm spectral energy distributions. From the emission-line strengths of these objects, we infer star formation rates of 10–25 M⊙ yr−1, while the lack of detections in the other objects imply even lower rates. By comparing our results with those of other authors, we conclude it is likely that the vast majority (more than 90 per cent) of the star formation in these objects is completely extinguished at rest-frame optical wavelengths, and the emission lines originate in a relatively unobscured region. Finally, we look at future prospects for making spectroscopic redshift determinations of submm galaxies.

We present a deep Infrared Space Observatory (ISO) observation at 6.7 μm of the 53W002 group of galaxies and active galactic nuclei (AGNs) at z = 2.4. This approximately samples the emitted K band. Faint, blue star‐forming objects are not detected, as expected from their very blue color across the emitted optical and UV spectrum. However, 53W002 itself is detected at the ∼3 σ level, with an emitted V−K color that is appropriate for a population that formed starting at z = 3.6–7.0, most likely z = 4.7. This fits with shorter wavelength data, suggesting that the more massive members of this group, which may all host AGNs, began star formation earlier in deeper potential wells than the compact Lyα emission objects. Two foreground galaxies are detected, as are several stars. One additional 6.7 μm source closely coincides with an optically faint galaxy, potentially at z = 2–3. The overall source counts are consistent (within the errors of such a small sample) with the other ISO deep fields at 6.7 μm.

We present new results from the SCUBA Local Universe Galaxy Survey, the first large statistical submillimetre survey of the local Universe. Following our initial survey of a sample of 104 IRAS-selected galaxies we now present the results of a sample of 80 Optically-selected galaxies. Since SCUBA is sensitive to the large proportion of dust too cold to be detected by IRAS the addition of this Optically-selected sample allows us for the first time to determine the amount of cold dust in galaxies of different Hubble types. We detect 6 ellipticals in the sample and find them to have dust masses in excess of 10^7 solar masses. We derive local submillimetre Luminosity Functions and Dust Mass functions, both directly for the Optically-Selected SLUGS sample and by extrapolation from the IRAS PSCz survey, and find them to be well-fitted by Schechter functions. We find excellent agreement between the two LFs and DMFs and show that, whereas the slope of the IRAS-selected LF at lower luminosities was steeper than -2 (a submm "Olbers' Paradox"), as expected the PSCz-extrapolated LF flattens out at the low luminosity end.

We present the X-ray source catalogues for the XMM surveys of the 3-h and 14-h Canada-France Redshift Survey fields (0.5-10 keV flux range similar to2 x 10(-15)-10(-13) erg cm(-2) s(-1)). We use a subset of the XMM sources, which have Chandra positions, to determine the best method of obtaining optical identifications of sources with only XMM positions. We find optical identifications for 79 per cent of the XMM sources for which there are deep optical images. The sources without optical identifications are likely to be optically fainter and have higher redshifts than the sources with identifications. We have estimated 'photometric redshifts' for the identified sources, calibrating our method using similar to200 galaxies in the fields with spectroscopic redshifts. We find that the redshift distribution has a strong peak at z similar to 0.7.The host galaxies of active galactic nuclei (AGN) identified in this work cover a wide range of optical properties, with every galaxy type being represented and no obvious preference for one type over another. Redder types tend to be more luminous than blue types, particularly at lower redshifts. The host galaxies also span a wide range of optical luminosity, in contrast to the narrow range found for the starburst galaxies detected in muJy radio surveys. We find a strong correlation between optical and X-ray luminosity similar to the Magorrian relation, although selection effects cannot be ruled out.

The timescales to replenish dust from the cool winds of asymptotic giant branch stars are believed to be greater than the timescales for dust destruction. In high-redshift galaxies, this problem is further compounded as the stars take longer than the age of the universe to evolve into the dust production stages. To explain these discrepancies, dust formation in supernovae (SNe) is required to be an important process, but until recently dust in supernova remnants (SNRs) has only been detected in very small quantities. We present the first submillimeter observations of cold dust in Kepler's SNR using the Submillimeter Common-User Bolometric Array. A two-component dust temperature model is required to fit the spectral energy distribution with Twarm ~ 102 K and Tcold ~ 17 K. The total mass of dust implied for Kepler is ~1 M☉—1000 times greater than previous estimates. Thus SNe, or their progenitors, may be important dust formation sites.

We present the complete submillimeter data for the Canada-UK Deep Submillimeter Survey (CUDSS) 3h field. The observations were taken with the Submillimeter Common-User Bolometric Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT) on Mauna Kea. The 3h field is one of two main fields in our survey and covers 60 arcmin2 to a 3 σ depth of ~3 mJy. In this field we have detected 27 sources above 3 σ and 15 above 3.5 σ. We assume that the differential source counts follow the form N(S) ∝ S-α and measure α = 3.3, in good agreement with previous studies. We estimate that SCUBA sources brighter than 3 mJy are responsible for ~13% of the extragalactic background at 850 μm (after correcting for flux boosting, 20% with no correction), which is in general agreement with previous estimates made by other groups. Using preliminary Infrared Space Observatory 15 μm maps and VLA 1.4 GHz data, we have identified counterparts for 10 objects and have detected two sources at 450 μm. With this information we estimate a lower limit on the median redshift of the sample of z > 1.4 with 6%-10% lying at z < 1. We have attempted to measure the angular clustering of S850 μm > 3 mJy sources using the source catalogs from the CUDSS two main fields, the 3h and 14h fields, and find ω(θ) = 4.4 ± 2.9θ-0.8, or a 3 σ upper limit on the clustering amplitude of less than 8.7 arcsec0.8. This is consistent with clustering at least as strong as that seen for the Lyman break galaxy population and the extremely red objects. Since SCUBA sources are selected over a broader range in redshifts than these two populations, the strength of the true spatial clustering is expected to be correspondingly stronger.