We report on the detection of a feature with negative radio flux in a sensitive, low resolution observation with the VLA. This morphologically peculiar feature is approximately 25" 65" in size with a ...peak central amplitude of about -0.25 mK compared to the brightness temperature of the background sky at 3.6 cm. Within about 1' of this microwave decrement, we also found two radio quiet quasars, both at 2.561, with a projected physical separation of about 1 Mpc (\(q_o\) = 0.5, h = 0.5), suggestive of a possible galaxy cluster in the region. We are unable to account for this negative source by systematic phase fluctuations within our observations, sidelobe artifacts, or instrumental noise. We discuss possible physical origins of this microwave source, in particular the inverse-Compton scattering of the cosmic microwave background by hot gas in a distant cluster of galaxies.
We describe the X-ray properties of a large sample of \(z\sim3\) Lyman Break Galaxies (LBGs) in the region of the Hubble Deep Field North, derived from the 1 Ms public Chandra observation. Of our ...sample of 148 LBGs, four are detected individually. This immediately gives a measure of the bright AGN fraction in these galaxies of \(\sim 3\)~per cent, which is in agreement with that derived from the UV spectra. The X-ray color of the detected sources indicates that they are probably moderately obscured. Stacking of the remainder shows a significant detection (\(6\sigma\)) with an average luminosity of \(3.5 \times 10^{41}\)~erg s\(^{-1}\) per galaxy in the rest frame 2-10 keV band. We have also studied a comparison sample of 95 z\(\sim 1\) ``Balmer Break'' galaxies. Eight of these are detected directly, with at least two clear AGN based on their high X-ray luminosity and very hard X-ray spectra respectively. The remainder are of relatively low luminosity (\(<10^{42}\)~erg s\(^{-1}\)), and the X-rays could arise from either AGN or rapid star-formation. The X-ray colors and evidence from other wavebands favor the latter interpretation. Excluding the clear AGN, we deduce a mean X-ray luminosity of \(6.6 \times 10^{40}\)~erg s\(^{-1}\), a factor \(\sim 5\) lower than the LBGs. The average ratio of the UV and X-ray luminosities of these starforming galaxies \(L_{\rm UV}/L_{\rm X}\), however, is approximately the same at \(z = 1\) as it is at \(z = 3\). This scaling implies that the X-ray emission follows the current star formation rate, as measured by the UV luminosity. We use our results to constrain the star formation rate at \(z\sim 3\) from an X-ray perspective (truncated).
We report on a complete sample of 7 luminous early-type galaxies in the Hubble Ultra Deep Field (UDF) with spectroscopic redshifts between 1.39 and 2.47 and to K<23 AB. Using the BzK selection ...criterion we have pre-selected a set of objects over the UDF which fulfill the photometric conditions for being passively evolving galaxies at z>1.4. Low-resolution spectra of these objects have been extracted from the HST+ACS grism data taken over the UDF by the GRAPES project. Redshift for the 7 galaxies have been identified based on the UV feature at rest frame 2640<lambda<2850 AA. This feature is mainly due to a combination of FeII, MgI and MgII absorptions which are characteristic of stellar populations dominated by stars older than about 0.5 Gyr. The redshift identification and the passively evolving nature of these galaxies is further supported by the photometric redshifts and by the overall spectral energy distribution (SED), with the ultradeep HST+ACS/NICMOS imaging revealing compact morphologies typical of elliptical/early-type galaxies. From the SED we derive stellar masses of 10^{11}Msun or larger and ages of about 1 Gyr. Their space density at < z >=1.7 appears to be roughly a factor of 2--3 smaller than that of their local counterparts, further supporting the notion that such massive and old galaxies are already ubiquitous at early cosmic times. Much smaller effective radii are derived for some of the objects compared to local massive ellipticals, which may be due to morphological K corrections, evolution, or the presence of a central point-like source. Nuclear activity is indeed present in a subset of the galaxies, as revealed by them being hard X-ray sources, hinting to AGN activity having played a role in discontinuing star formation.
1. We investigated the responses of cat lumbosacral Renshaw cells to pseudo-Poison stimulus sequences (of three different mean rates) delivered to motor axons in ventral roots or various muscle ...nerves. The Renshaw cell responses were evaluated by computation of peristimulus time histograms (PSTHs). 2. PSTHs computed with respect to all the stimuli showed, before the reference time, near-constant bin contents corresponding to the mean firing probability (rate), and an initial excitatory component (increase in discharge probability) after the reference time, followed by a small but longer-lasting reduction of firing rate. These two response components were strongly correlated linearly. It is suggested that the postexcitatory rate reduction is predominantly due to afterhyperpolarization. 3. In general, Renshaw cell responses to any stimulus in a stimulus train depended upon the stimulation history. In the averaged record, the response to the second of a pair of stimuli was affected by the first stimulus independently of intervening (random) stimuli. Very often, the second response showed a long-lasting depression (from 25 to greater than 250 ms). In a number of cases a briefer facilitating effect preceded the depression. 4. These conditioning effects were largely homosynaptic, i.e., confined to the particular input channel that was stimulated. This was shown by stimulating two different nerves (or nerve branches) with independent random patterns of similar mean rates and determining the cross-conditioning exerted by one input channel on the excitatory effects of the other. At small intervals between conditioning and test stimuli of some tens of milliseconds, a facilitatory effect could often be seen, which almost certainly reflected spatial summation. However, the subsequent depressant effect was largely accounted for by the postexcitatory rate reduction consequent to the conditioning stimulus in the parallel channel. Autoconditioning was still present. 5. The amount of facilitation and depression as well as their balance depended on the average Renshaw cell response. This in turn depended, at each mean stimulus rate, on the strength of synaptic coupling between an input channel and the cell, and on the mean stimulus rate, declining with an increase in mean rate. That is, the facilitation increased and the depression decreased with decreasing synaptic coupling and increasing mean stimulus rate. 6. Several factors may contribute to facilitation and depression; these are discussed with respect to their relative quantitative significance.
We report a sensitive search for redshifted CO (3-2) emission from the weak radio galaxy 53W002 at z=2.394. Maps at resolutions of 3 arcsec and 235km/s show a significant emission peak within 0.5 ...arcsec of the optical and radio continuum peaks. The measured narrow band flux is approximately ten times the extrapolated cm-wavelength non-thermal radio continuum expected at 101.9 GHz and exhibits a spectral profile implying a 540 km/s width (FWHM) at a systemic redshift z=2.394 for CO (3-2). This emission has a total integrated flux of 1.51(+/-0.2) Jy km/s, approximately four times weaker than that previously seen in the lensed systems FSC10214+4724 and the Cloverleaf QSO. For a Galactic CO-to-H2 conversion ratio, the implied molecular gas mass is 7.4x10^10 solar masses (H=75 km/s/Mpc and q=0.5). The CO emission is elongated at P.A.=120 degrees with a deconvolved major axis radius of 15 kpc (2.8 arcsec). This extension is along a similar direction to that seen in the cm-wave radio continuum and the optical but approximately three times larger. A velocity gradient is seen along the major axis, and if this structure is a (forming) disk, the implied dynamical mass is 9-22x10^10 solar masses at radii less than or equal to 15 kpc, assuming inclination i=0 degrees (edge-on). The magnitude of these masses and the similarity of the high gas-mass fraction are consistent with the host galaxy of 53W002 being a young galactic system, but the metallicity (probably greater than or equal to 0.1 solar in order to produce the CO lines) implies significant heavy element production prior to z=2.4. This constitutes the first high redshift molecular gas which is detected in emission where there is probably no gravitational magnification.
We demonstrate the ability to recover morphological luminosity distributions within medium redshift clusters (z ~ 0.55) based on Hubble Space Telescope WFPC2 observations. We postulate that a ...detailed survey of the morphological LDs in local, low and medium redshift clusters may provide strong constraints on the modes of galaxy evolution in rich clusters. Preliminary results suggest that in clusters, as also seen in the field, very strong evolution (i.e. dm = 2.5 mags since z = 0.55) is occurring in the late-type spiral and irregular populations.
Discharge patterns of group Ia afferents of muscle spindles in the (isometric) cat semitendinosus muscle were recorded when subjected to the influence of contractions of three motor units elicited by ...stimulation of three alpha-efferents with different regular or stochastic stimulus patterns. In order to study conditioning interactions between motor unit contractions, defined time constellations of stimuli to different motor units were isolated from the stimulus trains by electronic means. This technique was also applied to discharge patterns of two Ia fibres to isolate "correlated discharges." The effects of defined time constellations of stimuli upon discharge patterns of single Ia afferents or "correlated discharges" of pairs of Ia afferents were assessed by poststimulus time histograms (PSTHs). It turned out that the influence exerted by one motor unit on spindle discharges was more or less strongly modulated by actions of the other motor units, dependent on the relative timing of their contractions. These effects could in part be explained by the relative locations of motor units and spindles within the muscle. These results are discussed with respect to possible mechanisms of low-amplitude physiological tremor.
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