458 research outputs found
Refined procedures for accurate determination of solution structures of nucleic acids by two dimensional nuclear magnetic resonance spectroscopy
New procedures have been described for accurate determination of solution structures of nucleic acids. These are two fold; new two dimensional nuclear magnetic resonance techniques and better approaches for interpretation of nuclear magnetic resonance data for structure determination purposes. The significant development in two dimensional nuclear magnetic resonance techniques for this purpose are ω1 -scaling and recording of pure phase spectra. Use ofω1-scaled correlated and nuclear Overhauser effect spectra for estimation of interproton distances and 1H-1H coupling constants has been described. Computer simulation procedures for exact determination of structure have been described. Experimental spectra demonstrating the application of new procedures have been presented
Application of Resonance Perturbation Theory to Dynamics of Magnetization in Spin Systems Interacting with Local and Collective Bosonic Reservoirs
We apply our recently developed resonance perturbation theory to describe the
dynamics of magnetization in paramagnetic spin systems interacting
simultaneously with local and collective bosonic environments. We derive
explicit expressions for the evolution of the reduced density matrix elements.
This allows us to calculate explicitly the dynamics of the macroscopic
magnetization, including characteristic relaxation and dephasing time-scales.
We demonstrate that collective effects (i) do not influence the character of
the relaxation processes but merely renormalize the relaxation times, and (ii)
significantly modify the dephasing times, leading in some cases to a
complicated (time inhomogeneous) dynamics of the transverse magnetization,
governed by an effective time-dependent magnetic field
The Hawk-I UDS and GOODS Survey (HUGS): Survey design and deep K-band number counts
We present the results of a new, ultra-deep, near-infrared imaging survey
executed with the Hawk-I imager at the ESO VLT, of which we make all the data
public. This survey, named HUGS (Hawk-I UDS and GOODS Survey), provides deep,
high-quality imaging in the K and Y bands over the CANDELS UDS and GOODS-South
fields. We describe here the survey strategy, the data reduction process, and
the data quality. HUGS delivers the deepest and highest quality K-band images
ever collected over areas of cosmological interest, and ideally complements the
CANDELS data set in terms of image quality and depth. The seeing is exceptional
and homogeneous, confined to the range 0.38"-0.43". In the deepest region of
the GOODS-S field, (which includes most of the HUDF) the K-band exposure time
exceeds 80 hours of integration, yielding a 1-sigma magnitude limit of ~28.0
mag/sqarcsec. In the UDS field the survey matches the shallower depth of the
CANDELS images reaching a 1-sigma limit per sq.arcsec of ~27.3mag in the K band
and ~28.3mag in the Y-band, We show that the HUGS observations are well matched
to the depth of the CANDELS WFC3/IR data, since the majority of even the
faintest galaxies detected in the CANDELS H-band images are also detected in
HUGS. We present the K-band galaxy number counts produced by combining the HUGS
data from the two fields. We show that the slope of the number counts depends
sensitively on the assumed distribution of galaxy sizes, with potential impact
on the estimated extra-galactic background light (abridged).Comment: Accepted for publication on Astronomy and Astrophysic
GOODS-Herschel: star formation, dust attenuation, and the FIR-radio correlation on the main sequence of star-forming galaxies up to z=4
We use deep panchromatic data sets in the GOODS-N field, from GALEX to the deepest Herschel far-infrared (FIR) and VLA radio continuum imaging, to explore the evolution of star-formation activity and dust attenuation properties of star-forming galaxies to z sime 4, using mass-complete samples. Our main results can be summarized as follows: (i) the slope of the star-formation rateâM* correlation is consistent with being constant sime0.8 up to z sime 1.5, while its normalization keeps increasing with redshift; (ii) for the first time we are able to explore the FIRâradio correlation for a mass-selected sample of star-forming galaxies: the correlation does not evolve up to z sime 4; (iii) we confirm that galaxy stellar mass is a robust proxy for UV dust attenuation in star-forming galaxies, with more massive galaxies being more dust attenuated. Strikingly, we find that this attenuation relation evolves very weakly with redshift, with the amount of dust attenuation increasing by less than 0.3 mag over the redshift range [0.5â4] for a fixed stellar mass; (iv) the correlation between dust attenuation and the UV spectral slope evolves with redshift, with the median UV slope becoming bluer with redshift. By z sime 3, typical UV slopes are inconsistent, given the measured dust attenuations, with the predictions of commonly used empirical laws. (v) Finally, building on existing results, we show that gas reddening is marginally larger (by a factor of around 1.3) than the stellar reddening at all redshifts probed. Our results support a scenario where the ISM conditions of typical star-forming galaxies evolve with redshift, such that at z â„ 1.5 Main Sequence galaxies have ISM conditions moving closer to those of local starbursts
Calibrating Extinction-Free Star Formation Rate Diagnostics with 33GHz Free-Free Emission in NGC6946
Abridged: Using free-free emission measured in the Ka-band (26-40GHz) for 10
star-forming regions in the nearby galaxy NGC6946, including its starbursting
nucleus, we compare a number of SFR diagnostics that are typically considered
to be unaffected by interstellar extinction: i.e., non-thermal radio (i.e.,
1.4GHz), total infrared (IR; 8-1000um), and warm dust (i.e., 24um) emission,
along with the hybrid (obscured + unobscured) indicators of H\alpha+24um and
UV+IR. The 33GHz free-free emission is assumed to provide the most accurate
measure of the current SFR. Among the extranuclear star-forming regions, the
24um, H\alpha+24um and UV+IR SFR calibrations are in good agreement with the
33GHz free-free SFRs. However, each of the SFR calibrations relying on some
form of dust emission overestimate the nuclear SFR by a factor of ~2. This is
more likely the result of excess dust heating through an accumulation of
non-ionizing stars associated with an extended episode of star formation in the
nucleus rather than increased competition for ionizing photons by dust. SFR
calibrations using the non-thermal radio continuum yield values which only
agree with the free-free SFRs for the nucleus, and underestimate the SFRs from
the extranuclear star-forming regions by a factor of ~2. This result likely
arises from the CR electrons decaying within the starburst region with
negligible escape compared to the young extranuclear star-forming regions.
Finally, we find that the SFRs estimated using the total 33GHz emission agree
well with the free-free SFRs due to the large thermal fractions present at
these frequencies even when local diffuse backgrounds are not removed. Thus,
rest-frame 33GHz observations may act as a reliable method to measure the SFRs
of galaxies at increasingly high redshift without the need of ancillary radio
data to account for the non-thermal emission.Comment: 18 pages, 7 Figures, Accepted for publication in Ap
The Type Ia Supernova Rate in Radio and Infrared Galaxies from the CFHT Supernova Legacy Survey
We have combined the large SN Ia database of the Canada-France-Hawaii
Telescope Supernova Legacy Survey and catalogs of galaxies with photometric
redshifts, VLA 1.4 GHz radio sources, and Spitzer infrared sources. We present
eight SNe Ia in early-type host galaxies which have counterparts in the radio
and infrared source catalogs. We find the SN Ia rate in subsets of radio and
infrared early-type galaxies is ~1-5 times the rate in all early-type galaxies,
and that any enhancement is always <~ 2 sigma. Rates in these subsets are
consistent with predictions of the two component "A+B" SN Ia rate model. Since
infrared properties of radio SN Ia hosts indicate dust obscured star formation,
we incorporate infrared star formation rates into the "A+B" model. We also show
the properties of SNe Ia in radio and infrared galaxies suggest the hosts
contain dust and support a continuum of delay time distributions for SNe Ia,
although other delay time distributions cannot be ruled out based on our data.Comment: 14 pages, 6 figures, 7 tables, accepted for publication in A
Near-IR Search for Lensed Supernovae Behind Galaxy Clusters - II. First Detection and Future Prospects
Powerful gravitational telescopes in the form of massive galaxy clusters can
be used to enhance the light collecting power over a limited field of view by
about an order of magnitude in flux. This effect is exploited here to increase
the depth of a survey for lensed supernovae at near-IR wavelengths. A pilot SN
search program conducted with the ISAAC camera at VLT is presented. Lensed
galaxies behind the massive clusters A1689, A1835 and AC114 were observed for a
total of 20 hours split into 2, 3 and 4 epochs respectively, separated by
approximately one month to a limiting magnitude J<24 (Vega). Image subtractions
including another 20 hours worth of archival ISAAC/VLT data were used to search
for transients with lightcurve properties consistent with redshifted
supernovae, both in the new and reference data. The feasibility of finding
lensed supernovae in our survey was investigated using synthetic lightcurves of
supernovae and several models of the volumetric Type Ia and core-collapse
supernova rates as a function of redshift. We also estimate the number of
supernova discoveries expected from the inferred star formation rate in the
observed galaxies. The methods consistently predict a Poisson mean value for
the expected number of SNe in the survey between N_SN=0.8 and 1.6 for all
supernova types, evenly distributed between core collapse and Type Ia SN. One
transient object was found behind A1689, 0.5" from a galaxy with photometric
redshift z_gal=0.6 +- 0.15. The lightcurve and colors of the transient are
consistent with being a reddened Type IIP SN at z_SN=0.59. The lensing model
predicts 1.4 magnitudes of magnification at the location of the transient,
without which this object would not have been detected in the near-IR ground
based search described in this paper (unlensed magnitude J~25). (abridged)Comment: Accepted by AA, matches journal versio
Expectations of health care quality among rural Maya villagers in SololĂĄ Department, Guatemala: a qualitative analysis
A Multiwavelength Study of a Sample of 70 micron Selected Galaxies in the COSMOS Field I: Spectral Energy Distributions and Luminosities
We present a large robust sample of 1503 reliable and unconfused 70microm
selected sources from the multiwavelength data set of the Cosmic Evolution
Survey (COSMOS). Using the Spitzer IRAC and MIPS photometry, we estimate the
total infrared luminosity, L_IR (8--1000 microns), by finding the best fit
template from several different template libraries. The long wavelength 70 and
160 micron data allow us to obtain a reliable estimate of L_IR, accurate to
within 0.2 and 0.05 dex, respectively. The 70 micron data point enables a
significant improvement over the luminosity estimates possible with only a 24
micron detection. The full sample spans a wide range in L_IR, L_IR ~ 10^8-10^14
L_sun, with a median luminosity of 10^11.4 L_sun. We identify a total of 687
luminous, 303 ultraluminous, and 31 hyperluminous infrared galaxies (LIRGs,
ULIRGs, and HyLIRGs) over the redshift range 0.01<z<3.5 with a median redshift
of 0.5. Presented here are the full spectral energy distributions for each of
the sources compiled from the extensive multiwavelength data set from the
ultraviolet (UV) to the far-infrared (FIR). Using SED fits we find possible
evidence for a subset of cooler ultraluminous objects than observed locally.
However, until direct observations at longer wavelengths are obtained, the peak
of emission and the dust temperature cannot be well constrained. We use these
SEDs, along with the deep radio and X-ray coverage of the field, to identify a
large sample of candidate active galactic nuclei (AGN). We find that the
fraction of AGN increases strongly with L_IR, as it does in the local universe,
and that nearly 70% of ULIRGs and all HyLIRGs likely host a powerful AGN.Comment: 31 pages including 31 figures and 6 tables. Accepted for publication
in ApJ. The full resolution version is available here:
http://www.ifa.hawaii.edu/~jeyhan/paperI/Kartaltepe_70mic_PaperI.pd
- âŠ