On the Origins of Cosmic Dust and the Evolution of Nearby Galaxies with the Herschel Space Observatory

Using multiwavelength observations, centred around the unique far-infrared and submillimetre window provided by the Herschel Space Observatory, this thesis investigates the origins and evolution of cosmic dust in the local Universe – by examining individual sources of dust in our own galaxy, and by studying dust in nearby galaxies. I search Herschel observations of the remnants of Kepler’s (SN1604) and Tycho’s (SN1572) supernovæ, both Type-Ia explosions, for evidence of dust creation by these events. Being the only Type-Ia supernovæ known to have occurred in our Galaxy within the past 1,000 years, these remnants are the only ones both close enough to resolve, and young enough that they are dominated by their ejecta dynamics. There is no indication of any recently manufactured dust associated with either supernova remnant. It therefore appears that Type-Ia supernovæ do not contribute significantly to the dust budgets of galaxies. The Crab Nebula, the result of a Type-II supernova (SN1054), is also investigated using Herschel and multiwavelength data. After accounting for other sources of emission, a temperature of Td = 63.1 K and mass of Md = 0.21 M⊙ is derived for the Crab Nebula’s dust component. I create a map of the distribution of dust in the Crab Nebula, the first of its kind, by means of a resolved component separation, revealing that the dust is located in the dense filamentary ejecta. We can be confident that this dust will survive in the long term, and be injected into the galactic dust budget. This is the first detection of manufactured supernova dust for which this can be said. Next I use the Herschel-ATLAS to assemble HAPLESS: the Herschel- ATLAS Phase-1 Limited Extent Spatial Sample – a blind, volume-limited, dust- selected sample of nearby galaxies. The majority of this sample is made up of curious very blue galaxies. Often irregular and/or flocculent in morphology, with extremely blue UV-NIR colours, these galaxies appear to be prominent in the local dusty universe. In the absence of reliable photometry for the HAPLESS galaxies, I describe the function and testing of a purpose-built photometric pipeline – CAAPR: Chris’ Adequate Aperture Photometry Routine. The photometry conducted with CAAPR exhibits flux greater by factors of, on average, 1.6 in the FUV and 1.4 in r-band, relative to the previously-available photometry. In comparison to other surveys of dust in local galaxies, the HAPLESS systems show a strong propensity towards very late morphological types and extremely blue FUV-Ks colours. The dust in the HAPLESS galaxies appears to be very cold, with a median temperature of 14.6 K. They are also exceptionally dust rich, with a median dust mass of 5.3 × 106 M$_{\odot}$ , and a median Md/M$_{\star}$ of 4.4×10-3 – greater by a factor of 1.8–3.7 than that seen in other local surveys. The curious very blue HAPLESS galaxies, whilst accounting for only 6% of the stellar mass in our sample, contain over 35% of the dust mass. I show that the more dust-rich a galaxy (as defined by Md/M$_{\star}$), the smaller the fraction of its UV luminosity that suffers dust absorption – this effect is observed to be particularly dramatic in the case of the curious very blue objects. Either the emissivity or geometry of the dust in these systems must be highly unusual. HAPLESS suggests a dust mass volume density of the local universe of (3.7 ± 0.7) × 105 M$_{\odot}$ Mpc-3; the largest value reported to date. The HAPLESS 250 μm luminosity function is in good agreement with surveys of far larger volumes, suggesting that we do not sample an over-dense region of space. The HAPLESS galaxies are extraordinarily gas rich; the median HAPLESS gas fraction is 0.52, and 19% of the sample have gas fractions >0.8. The median HAPLESS gas-to-dust ratio is ≈260, 2–3 times larger than in other local surveys. The very blue galaxies of the sample are found to be particularly gas rich; a chemical and dust evolution model indicates that they are at an early stage of converting their gas into stars. A dust-selected survey such as H-ATLAS is a particularly efficient way of identifying young systems of this kind, which should therefore provide valuable insights into the chemical evolution of young galaxies

An empirical determination of the dust mass absorption coefficient, κd, using the Herschel Reference Survey

We use the published photometry and spectroscopy of 22 galaxies in the Herschel Reference Survey to determine that the value of the dust mass absorption coefficient κ d at a wavelength of 500 μm is κ500 = (0.051 +0.070 −0.026) m^2 kg^-1. We do so by taking advantage of the fact that the dust-to-metals ratio in the interstellar medium of galaxies appears to be constant. We argue that our value for κd supersedes that of James et al. (2002) – who pioneered this approach for determining κd – because we take advantage of superior data, and account for a number of significant systematic effects that they did not consider. We comprehensively incorporate all methodological and observational contributions to establish the uncertainty on our value, which represents a marked improvement on the oft-quoted ‘order-of-magnitude’ uncertainty on κd . We find no evidence that the value of κd differs significantly between galaxies, or that it correlates with any other measured or derived galaxy properties. We note, however, that the availability of data limits our sample to relatively massive (10^9.7 < Mstar < 10&11.0 Msol ), high metallicity (8.61 < [12 + log 10 O/H] < 8.86) galaxies; future work will allow us to investigate a wider range of systems

Controls on preservation of organic matter during the Cenomanian Ocean Anoxic Event II (OAE2) and Turonian global sea-level rise: Agadir Basin, Morocco

The Ocean Anoxic Event II (OAE2) was a significant global event associated with a positive carbon isotope excursion, occurring from the Late Cenomanian to the Early Turonian (C/T). It has been commonly associated with enhanced organic carbon preservation. Carbon isotopic analysis carried out over the C/T interval in the Agadir Basin, Morocco, integrated with previous biostratigraphic data, allows a refined correlation of the OAE2 interval. Detailed sedimentary facies analysis identifies ten lithofacies that record the transition from shallow marine environments in the Late Cenomanian to relatively deeper conditions in the Early Turonian. The variation in lithofacies can be correlated to relative sea level changes that show a correlation to the global eustatic curve. The OAE2 interval comprises dark grey mudstones beds that display low total organic carbon (TOC) values. Trace element and facies analysis suggest dilution from high detrital influx, along with oxic water conditions and low productivity. OM-rich black mudstones are identified in post-OAE2 Early Turonian strata. Trace element analysis suggests this increase in organic matter accumulation was related to increased sea surface productivity and oxygen-depleted bottom water conditions, which facilitated organic matter preservation. Deposition of OM-rich black mudstones is widely reported during the global Early Turonian marine transgression, suggesting the very high sea level was a major control on organic matter generation and preservation

On the origins of cosmic dust and the evolution of nearby galaxies with the Herschel Space Observatory

USING multiwavelength observations, centred around the unique far-infrared and submillimetre window provided by the Herschel Space Observatory, this thesis investigates the origins and evolution of cosmic dust in the local Universe – by examining individual sources of dust in our own galaxy, and by studying dust in nearby galaxies. Herschel observations of the remnants of Kepler’s (SN1604) and Tycho’s (SN1572) supernovae, both Type-Ia explosions, are searched for evidence of dust creation by these events. Being the only Type-Ia supernovae known to have occurred in our Galaxy within the past 1,000 years, these remnants are the only ones both close enough to resolve, and young enough that they are dominated by their ejecta dynamics. There is no indication of any recently manufactured dust associated with either supernova remnant. It therefore appears that Type-Ia supernovae do not contribute significantly to the dust budgets of galaxies. The Crab Nebula, the result of a Type-II supernova (SN1054), is also investigated using Herschel and multiwavelength data. After accounting for other sources of emission, a temperature of Td = 63.1K and mass of Md = 0.21M⊙ is derived for the Crab Nebula’s dust component. A map of the distribution of dust in the Crab Nebula, the first of its kind, is created by means of a resolved component separation, revealing that the dust is located in the dense filamentary ejecta. We can be confident that this dust will survive in the long term, and be injected into the galactic dust budget. This is the first detection of manufactured supernova dust for which this can be said. I next use the Herschel-ATLAS to assemble HAPLESS: the Herschel-ATLAS Phase-1 Limited Extent Spatial Sample – a blind, volume-limited, dust-selected sample of nearby galaxies. The majority of this sample is made up of curious very blue UV-NIR colours, these galaxies appear to be prominent in the local dusty universe. In the absence of reliable photometry for the HAPLESS galaxies, I describe the function and testing of a purpose-built photometric pipeline – CAAPR: Chris’ Adequate Aperture Photometry Routine. The photometry conducted with CAAPR exhibits flux greater by factors of, on average, 1.6 in the FUV and 1.4 in r-band, relative to the previously-available photometry. In comparison to other surveys of dust in local galaxies, the HAPLESS systems show a strong propensity towards very late morphological types and extremely blue FUV-KS colours. The dust in the HAPLESS galaxies appears to be very cold, with a median temperature of 14.6 K. They are also exceptionally dust rich, with a median dust mass of 5.3�106M⊙, and a median Md/M⋆ of 4.4�1