Citation for published item:svisonD FtF nd vewisD eFtFF nd eissD eF nd erumugmD F nd impsonD tFwF nd rollndD FF nd wddoxD F nd hunneD vF nd linteD iF nd vn der erfD F nd ymontD eF nd hnneruerD rF nd milD sF nd fertoldiD pF nd fremerD wF nd fussmnnD FF nd giD FEF nd glementsD hFvF nd gooryD eF nd he ottiD qF nd ilesD FeF nd pullerD gF nd qonzlezExuevoD tF nd srD iF nd xegrelloD wF nd yteoD sF nd ¡ erezEpournonD sF nd iehersD hF nd tevensD tFeF nd winnkD eFwF nd rdlowD tF @PHITA 9he spe density of luminous dusty strEforming glxies t z b R X gfeEP nd vefyge imging of ultrred glxies from rershelEeveF9D estrophysil journlFD VQP @IAF pF UVF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACT Until recently, only a handful of dusty, star-forming galaxies (DSFGs) were known at z>4, most of them significantly amplified by gravitational lensing. Here, we have increased the number of such DSFGs substantially, selecting galaxies from the uniquely wide 250, 350, and 500 μm Herschel-ATLAS imaging survey on the basis of their extremely red far-infrared colors and faint 350 and 500 μm flux densities, based on which, they are expected to be largely unlensed, luminous, rare, and very distant. The addition of ground-based continuum photometry at longer wavelengths from the James Clerk Maxwell Telescope and the Atacama Pathfinder Experiment allows us to identify the dust peak in their spectral energy distributions (SEDs), with which we can better constrain their redshifts. We select the SED templates that are best able to determine photometric redshifts using a sample of 69 high-redshift, lensed DSFGs, then perform checks to assess the impact of the CMB on our technique, and to quantify the systematic uncertainty associated with our photometric redshifts, σ=0.14 (1 + z), using a sample of 25 galaxies with spectroscopic redshifts, each consistent with our color selection. For Herschel-selected ultrared galaxies with typical colors of S 500 /S 250 ∼2.2 and S 500 /S 350 ∼1.3 and flux densities, S 500 ∼50 mJy, we determine a median redshift, = z 3.66 phot , an interquartile redshift range, 3.30-4.27, with a median rest-frame 8-1000 μm luminosity, L IR , of 1.3× 1013 L e . A third of the galaxies lie at z>4, suggesting a space density, ρ z>4 , of ≈6×10 −7 Mpc −3 . Our sample contains the most luminous known star-forming galaxies, and the most overdense cluster of starbursting proto-ellipticals found to date.

We present Herschel/PACS 100 and 160 µm integrated photometry for the 323 galaxies in the Herschel Reference Survey (HRS), a K-band-, volume-limited sample of galaxies in the local Universe. Once combined with the Herschel/SPIRE observations already available, these data make the HRS the largest representative sample of nearby galaxies with homogeneous coverage across the 100-500 µm wavelength range. In this paper, we take advantage of this unique dataset to investigate the properties and shape of the far-infrared/sub-millimeter spectral energy distribution in nearby galaxies. We show that, in the stellar mass range covered by the HRS (8 < ∼log(M * /M ⊙ ) < ∼12), the farinfrared/sub-millimeter colours are inconsistent with a single modified black-body having the same dust emissivity index β for all galaxies. In particular, either β decreases, or multiple temperature components are needed, when moving from metal-rich/gaspoor to metal-poor/gas-rich galaxies. We thus investigate how the dust temperature and mass obtained from a single modified black-body depend on the assumptions made on β. We show that, while the correlations between dust temperature, galaxy structure and star formation rate are strongly model dependent, the dust mass scaling relations are much more reliable, and variations of β only change the strength of the observed trends. c 0000 RAS 2 L. Cortese et al.

Herschel FIR observations are used to construct Virgo cluster galaxy luminosity functions and to show that the cluster lacks the very bright and the numerous faint sources detected in field galaxy surveys. The far-infrared SEDs are fitted to obtain dust masses and temperatures and the dust mass function. The cluster is over dense in dust by about a factor of 100 compared to the field. The same emissivity (β) temperature relation applies for different galaxies as that found for different regions of M31. We use optical and HI data to show that Virgo is over dense in stars and atomic gas by about a factor of 100 and 20 respectively. Metallicity values are used to measure the mass of metals in the gas phase. The mean metallicity is ∼ 0.7 solar and ∼50% of the metals are in the dust. For the cluster as a whole the mass density of stars in galaxies is 8 times that of the gas and the gas mass density is 130 times that of the metals. We use our data to consider the chemical evolution of the individual galaxies, inferring that the measured variations in effective yield are due to galaxies having different ages, being affected to varying degrees by gas loss. Four galaxy scaling relations are considered: mass-metallicity, mass-velocity, mass-star formation rate and mass-radius -we suggest that initial galaxy mass is the prime driver of a galaxy's ultimate destiny. Finally, we use X-ray observations and galaxy dynamics to assess the dark and baryonic matter content compared to the cosmological model.

The Herschel Fornax Cluster Survey (HeFoCS) is a deep, far-infrared (FIR) survey of the Fornax cluster. The survey is in 5 Herschel bands (100 -500 µm) and covers an area of 16 deg 2 centred on NGC 1399. This paper presents photometry, detection rates, dust masses and temperatures using an optically selected sample from the Fornax Cluster Catalogue (FCC). Our results are compared with those previously obtained using data from the Herschel Virgo Cluster Survey (HeViCS). In Fornax, we detect 30 of the 237 (13 %) optically selected galaxies in at least one Herschel band. The global detection rates are significantly lower than Virgo, reflecting the morphological make up of each cluster -Fornax has a lower fraction of late-type galaxies. For galaxies detected in at least 3 bands we fit a modified blackbody with a β = 2 emissivity. Detected early-type galaxies (E / S0) have a mean dust mass, temperature, and dustto-stars ratio of log 10 (< M dust > /M ) = 5.82 ± 0.20, < T dust >= 20.82 ± 1.77 K, and log 10 (M dust /M stars ) = −3.87 ± 0.28, respectively. Late-type galaxies (Sa to Sd) have a mean dust mass, temperature, and dust-to-stars ratio of log 10 (< M dust > /M ) = 6.54 ± 0.19, < T dust >= 17.47 ± 0.97 K, and log 10 (M dust /M stars ) = −2.93 ± 0.09, respectively. The different cluster environments seem to have had little effect on the FIR properties of the galaxies and so we conclude that any environment dependent evolution, has taken place before the cluster was assembled. Drinkwater et al. (2001) showed that despite Fornax's apparent state of relaxation, it still contains substructure, e.g. a small, in-falling group centred on NGC 1316, 3 • to the southwest. However, compared to the Virgo cluster, Fornax is very centrally concentrated and probably at a much later epoch of formation. This is also suggested by the strong morphological segregation that has taken place, leaving the cluster almost entirely composed of early-type galaxies. Drinkwater et al. (2001) also noted that there exist two different populations, suggesting that while the giant galaxies are virialised, the dwarf population is still in-falling.

Surrounding the Milky Way (MW) is the circumgalactic medium (CGM), an extended reservoir of hot gas that has significant implications for the evolution of the MW. We used the HaloSat all-sky survey to study the CGM’s soft X-ray emission in order to better define its distribution and structure. We extend a previous HaloSat study of the southern CGM (Galactic latitude b < −30°) to include the northern CGM (b > 30°) and find evidence that at least two hot gas model components at different temperatures are required to produce the observed emission. The cooler component has a typical temperature of kT ∼0.18 keV, while the hotter component has a typical temperature of kT ∼0.7 keV. The emission measure in both the warm and hot components has a wide range (∼0.005–0.03, and ∼0.0005–0.004 cm−6 pc, respectively), indicating that the CGM is clumpy. A patch of relatively consistent CGM was found in the north, allowing for the CGM spectrum to be studied in finer detail using a stacked spectrum. The stacked spectrum is well described with a model including two hot gas components at temperatures of kT = 0.166 ± 0.005 keV and kT = 0.69 − 0.05 + 0.04 keV. As an alternative to adding a hot component, a neon-enhanced single-temperature model of the CGM was also tested and found to have worse fit statistics and poor residuals.