Gravitational Lensing at Millimeter Wavelengths

With today's millimeter and submillimeter instruments observers use gravitational lensing mostly as a tool to boost the sensitivity when observing distant objects. This is evident through the dominance of gravitationally lensed objects among those detected in CO rotational lines at z>1. It is also evident in the use of lensing magnification by galaxy clusters in order to reach faint submm/mm continuum sources. There are, however, a few cases where millimeter lines have been directly involved in understanding lensing configurations. Future mm/submm instruments, such as the ALMA interferometer, will have both the sensitivity and the angular resolution to allow detailed observations of gravitational lenses. The almost constant sensitivity to dust emission over the redshift range z=1-10 means that the likelihood for strong lensing of dust continuum sources is much higher than for optically selected sources. A large number of new strong lenses are therefore likely to be discovered with ALMA, allowing a direct assessment of cosmological parameters through lens statistics. Combined with an angular resolution <0.1", ALMA will also be efficient for probing the gravitational potential of galaxy clusters, where we will be able to study both the sources and the lenses themselves, free of obscuration and extinction corrections, derive rotation curves for the lenses, their orientation and, thus, greatly constrain lens models.Comment: 69 pages, Review on quasar lensing. Part of a LNP Topical Volume on "Dark matter and gravitational lensing", eds. F. Courbin, D. Minniti. To be published by Springer-Verlag 2002. Paper with full resolution figures can be found at ftp://oden.oso.chalmers.se/pub/tommy/mmviews.ps.g

Witnessing the Birth of the Red Sequence: ALMA High-resolution Imaging of [C II] and Dust in Two Interacting Ultra-red Starbursts at z = 4.425

Exploiting the sensitivity and spatial resolution of the Atacama Large Millimeter/submillimeter Array, we have studied the morphology and the physical scale of the interstellar medium—both gas and dust—in SGP 38326, an unlensed pair of interacting starbursts at z = 4.425. SGP 38326 is the most luminous star bursting system known at z > 4, with a total IR luminosity of L IR ~ 2.5 × 1013 L ⊙ and a star formation rate of ~ 4500 M ⊙ yr−1. SGP 38326 also contains a molecular gas reservoir among the most massive yet found in the early universe, and it is the likely progenitor of a massive, red-and-dead elliptical galaxy at z ~ 3. Probing scales of ~0farcs1 or ~800 pc we find that the smooth distribution of the continuum emission from cool dust grains contrasts with the more irregular morphology of the gas, as traced by the [C ii] fine structure emission. The gas is also extended over larger physical scales than the dust. The velocity information provided by the resolved [C ii] emission reveals that the dynamics of the two interacting components of SGP 38326 are each compatible with disk-like, ordered rotation, but also reveals an ISM which is turbulent and unstable. Our observations support a scenario where at least a subset of the most distant extreme starbursts are highly dissipative mergers of gas-rich galaxies

Observations of the High Redshift Universe

(Abridged) In these lectures aimed for non-specialists, I review progress in understanding how galaxies form and evolve. Both the star formation history and assembly of stellar mass can be empirically traced from redshifts z~6 to the present, but how the various distant populations inter-relate and how stellar assembly is regulated by feedback and environmental processes remains unclear. I also discuss how these studies are being extended to locate and characterize the earlier sources beyond z~6. Did early star-forming galaxies contribute significantly to the reionization process and over what period did this occur? Neither theory nor observations are well-developed in this frontier topic but the first results presented here provide important guidance on how we will use more powerful future facilities.Comment: To appear in `First Light in Universe', Saas-Fee Advanced Course 36, Swiss Soc. Astrophys. Astron. in press. 115 pages, 64 figures (see http://www.astro.caltech.edu/~rse/saas-fee.pdf for hi-res figs.) For lecture ppt files see http://obswww.unige.ch/saas-fee/preannouncement/course_pres/overview_f.htm

Clarifying the nature of the brightest submillimetre sources: interferometric imaging of LH850.02

We present high-resolution interferometric imaging of LH850.02, the brightest 850- and 1200-micron submillimetre (submm) galaxy in the Lockman Hole. Our observations were made at 890 micron with the Submillimetre Array (SMA). Our high-resolution submm imaging detects LH850.02 at >6-sigma as a single compact (size < 1 arcsec or < 8 kpc) point source and yields its absolute position to ~0.2-arcsec accuracy. LH850.02 has two alternative radio counterparts within the SCUBA beam (LH850.02N & S), both of which are statistically very unlikely to be so close to the SCUBA source position by chance. However, the precise astrometry from the SMA shows that the submm emission arises entirely from LH850.02N, and is not associated with LH850.02S (by far the brighter of the two alternative identifications at 24-micron). Fits to the optical-infrared multi-colour photometry of LH850.02N & S indicate that both lie at z~3.3, and are therefore likely to be physically associated. At these redshifts, the 24 micron--to--submm flux density ratios suggest that LH850.02N has an Arp220-type starburst-dominated far-IR SED, while LH850.02S is more similar to Mrk231, with less dust-enshrouded star-formation activity, but a significant contribution at 24-micron (rest-frame ~5-6 micron) from an active nucleus. This complex mix of star-formation and AGN activity in multi-component sources may be common in the high redshift ultraluminous galaxy population, and highlights the need for precise astrometry from high resolution interferometric imaging for a more complete understanding.Comment: MNRAS, in pres

The SCUBA HAlf Degree Extragalactic Survey (SHADES) - V. Submillimetre properties of near-infrared-selected galaxies in the Subaru/XMM -Newton deep field

We have studied the submillimetre ( submm) properties of the following classes of near- infraredselected ( NIR- selected) massive galaxies at high redshifts: BzK- selected star- forming galaxies ( BzKs); distant red galaxies ( DRGs); and extremely red objects ( EROs). We used the SCUBA HAlf Degree Extragalactic Survey ( SHADES), the largest uniform submm survey to date. Partial overlap of SIRIUS/ NIR images and SHADES in Subaru/ XMM - Newton deep field has allowed us to identify four submm- bright NIR- selected galaxies, which are detected in the mid- IR, 24 m, and the radio, 1.4 GHz. We find that all of our submm- bright NIR- selected galaxies satisfy the BzK selection criteria, i. e. BzK = ( z - K) AB - ( B - z) AB >= - 0.2, except for one galaxy whose B - z and z - K colours are however close to the BzK colour boundary. Two of the submm- bright NIR- selected galaxies satisfy all of the selection criteria we considered, i. e. they belong to the BzK - DRG - ERO overlapping population, or ` extremely red' BzKs. Although these extremely red BzKs are rare ( 0.25 arcmin(-2)), up to 20 per cent of this population could be submm galaxies. This fraction is significantly higher than that found for other galaxy populations studied here. Via a stacking analysis, we have detected the 850- mu m flux of submm- faint BzKs and EROs in our SCUBAmaps. While the contribution of z similar to 2 BzKs to the submm background is about 10 - 15 per cent and similar to that from EROs typically at z similar to 1, BzKs have a higher fraction (similar to 30 per cent) of submm flux in resolved sources compared with EROs and submm sources as a whole. From the spectral energy distribution ( SED) fitting analysis for both submm- bright and submm- faint BzKs, we found no clear signature that submm- bright BzKs are experiencing a specifically luminous evolutionary phase, compared with submm- faint BzKs. An alternative explanation might be that submm- bright BzKs are more massive than submm- faint ones

Reflections on designing a Biology/Humanities interdisciplinary module

This paper uses the reflections of a recent workshop on biology and the humanities subject areas to consider the potential for designing a first year interdisciplinary module that brings together teachers and learners in the Biosciences with their counterparts in English and History. It considers three building blocks of module design: aims and objectives; teaching and learning strategies; and assessment; and provides a commentary on the discussion of interdisciplinarity in the broader literature. The authors argue that interdisciplinary teaching and learning must be transformative, but not in the way many previous advocates of interdisciplinarity have assumed. Rather than transcending disciplines, the authors contend that the aim should be to enhance disciplinary understanding. Learners should emerge from the interdisciplinary module not having lost their identity as biologists, but having enhanced it. They should have become ‘better’ biologists in the sense of having developed a broader, critical understanding of the precepts of their discipline, as a first step to an understanding of biology inflected with a literary and historical awareness