Search for Inclusive b → sl^+l^-

We have searched for the effective flavor changing neutral-current decays b→sl^+l^- using an inclusive method. We set upper limits on the branching ratios B(b→se^+e^-)<5.7×10^(-5), B(b→sμ^+μ^-)<5.8×10^(-5), and B(b→se^±μ^∓)<2.2×10^(-5) [at 90% confidence level (C.L.)]. Combing the dielectron and dimuon decay modes we find B(b→sl^+l^-)<4.2×10^(-5) (at 90% C.L.)

Microwave Kinetic Inductance Detector (MKID) Camera Testing for Submillimeter Astronomy

Developing kilopixel focal planes for incoherent submm- and mm-wave detectors remains challenging due to either the large hardware overhead or the complexity of multiplexing standard detectors. Microwave kinetic inductance detectors (MKIDs) provide a efficient means to produce fully lithographic background-limited kilopixel focal planes. We are constructing an MKID-based camera for the Caltech Submillimeter Observatory with 576 spatial pixels each simultaneously sensitive in 4 bands at 230, 300, 350, and 400 GHz. The novelty of MKIDs has required us to develop new techniques for detector characterization. We have measured quasiparticle lifetimes and resonator Qs for detector bath temperatures between 200 mK and 400 mK. Equivalent lifetime measurements were made by coupling energy into the resonators either optically or by driving the third harmonic of the resonator. To determine optical loading, we use both lifetime and internal Q measurements, which range between 15,000 and 30,000 for our resonators. Spectral bandpass measurements confirm the placement of the 230 and 350 GHz bands. Additionally, beam maps measurements conform to expectations. The same device design has been characterized on both sapphire and silicon substrates, and for different detector geometries. We also report on the incorporation of new shielding to reduce detector sensitivity to local magnetic fields

A Unifying Model of Genome Evolution Under Parsimony

We present a data structure called a history graph that offers a practical basis for the analysis of genome evolution. It conceptually simplifies the study of parsimonious evolutionary histories by representing both substitutions and double cut and join (DCJ) rearrangements in the presence of duplications. The problem of constructing parsimonious history graphs thus subsumes related maximum parsimony problems in the fields of phylogenetic reconstruction and genome rearrangement. We show that tractable functions can be used to define upper and lower bounds on the minimum number of substitutions and DCJ rearrangements needed to explain any history graph. These bounds become tight for a special type of unambiguous history graph called an ancestral variation graph (AVG), which constrains in its combinatorial structure the number of operations required. We finally demonstrate that for a given history graph $G$, a finite set of AVGs describe all parsimonious interpretations of $G$, and this set can be explored with a few sampling moves.Comment: 52 pages, 24 figure

X-ray induced fragmentation of size-selected salt cluster-ions stored in an ion trap

Peer reviewe

American Astronomical Society logo iop-2016.png Nature of Faint Radio Sources in GOODS-North and GOODS-South Fields. I. Spectral Index and Radio–FIR Correlation

We present the first results from the deep and wide 5 GHz radio observations of the Great Observatories Origins Deep Survey (GOODS)-North (σ = 3.5 μJy beam−1, synthesized beam size θ = 147 × 142, and 52 sources over 109 arcmin2) and GOODS-South (σ = 3.0 μJy beam−1, θ = 098 × 045, and 88 sources over 190 arcmin2) fields using the Karl G. Jansky Very Large Array. We derive radio spectral indices α between 1.4 and 5 GHz using the beam-matched images and show that the overall spectral index distribution is broad even when the measured noise and flux bias are considered. We also find a clustering of faint radio sources around α = 0.8, but only within S 5 GHz \u3c 150 μJy. We demonstrate that the correct radio spectral index is important for deriving accurate rest-frame radio power and analyzing the radio–FIR correlation, and adopting a single value of α = 0.8 leads to a significant scatter and a strong bias in the analysis of the radio–FIR correlation, resulting from the broad and asymmetric spectral index distribution. When characterized by specific star formation rates, the starburst population (58%) dominates the 5 GHz radio source population, and the quiescent galaxy population (30%) follows a distinct trend in spectral index distribution and the radio–FIR correlation. Lastly, we offer suggestions on sensitivity and angular resolution for future ultra-deep surveys designed to trace the cosmic history of star formation and AGN activity using radio continuum as a probe

Genomic Organization of Duplicated Major Histocompatibility Complex Class I Regions in Atlantic Salmon (Salmo Salar)

Background: We have previously identified associations between major histocompatibility complex(MHC) class I and resistance towards bacterial and viral pathogens in Atlantic salmon. To evaluate if onlyMHC or also closely linked genes contributed to the observed resistance we ventured into sequencing ofthe duplicated MHC class I regions of Atlantic salmon.Results: Nine BACs covering more than 500 kb of the two duplicated MHC class I regions of Atlanticsalmon were sequenced and the gene organizations characterized. Both regions contained the proteasomecomponents PSMB8, PSMB9, PSMB9-like and PSMB10 in addition to the transporter for antigen processingTAP2, as well as genes for KIFC1, ZBTB22, DAXX, TAPBP, BRD2, COL11A2, RXRB and SLC39A7. TheIA region contained the recently reported MHC class I Sasa-ULA locus residing approximately 50 kbupstream of the major Sasa-UBA locus. The duplicated class IB region contained an MHC class I locusresembling the rainbow trout UCA locus, but although transcribed it was a pseudogene. No other MHCclass I-like genes were detected in the two duplicated regions. Two allelic BACs spanning the UBA locushad 99.2% identity over 125 kb, while the IA region showed 82.5% identity over 136 kb to the IB region.The Atlantic salmon IB region had an insert of 220 kb in comparison to the IA region containing threechitin synthase genes.Conclusion: We have characterized the gene organization of more than 500 kb of the two duplicatedMHC class I regions in Atlantic salmon. Although Atlantic salmon and rainbow trout are closely related,the gene organization of their IB region has undergone extensive gene rearrangements. The Atlanticsalmon has only one class I UCA pseudogene in the IB region while trout contains the four MHC UCA, UDA,UEA and UFA class I loci. The large differences in gene content and most likely function of the salmon andtrout class IB region clearly argues that sequencing of salmon will not necessarily provide informationrelevant for trout and vice versa

Nature of Faint Radio Sources in GOODS-North and GOODS-South Fields – I. Spectral Index and Radio-FIR Correlation

We present the first results from the deep and wide 5 GHz radio observations of the Great Observatories Origins Deep Survey (GOODS)-North (σ = 3.5 μJy beam−1, synthesized beam size θ = 147 × 142, and 52 sources over 109 arcmin2) and GOODS-South (σ = 3.0 μJy beam−1, θ = 098 × 045, and 88 sources over 190 arcmin2) fields using the Karl G. Jansky Very Large Array. We derive radio spectral indices α between 1.4 and 5 GHz using the beam-matched images and show that the overall spectral index distribution is broad even when the measured noise and flux bias are considered. We also find a clustering of faint radio sources around α = 0.8, but only within S 5 GHz \u3c 150 μJy. We demonstrate that the correct radio spectral index is important for deriving accurate rest-frame radio power and analyzing the radio–FIR correlation, and adopting a single value of α = 0.8 leads to a significant scatter and a strong bias in the analysis of the radio–FIR correlation, resulting from the broad and asymmetric spectral index distribution. When characterized by specific star formation rates, the starburst population (58%) dominates the 5 GHz radio source population, and the quiescent galaxy population (30%) follows a distinct trend in spectral index distribution and the radio–FIR correlation. Lastly, we offer suggestions on sensitivity and angular resolution for future ultra-deep surveys designed to trace the cosmic history of star formation and AGN activity using radio continuum as a probe

Stellar Half-Mass Radii of 0.5<z<2.30.5<z<2.3 Galaxies: Comparison with JWST/NIRCam Half-Light Radii

We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of $>$500 $M_\star>10^{10}~M_\odot$ galaxies in the redshift range $0.5<z<2.3$. We compare the resulting rest-frame 1.5-2$\mu$m half-light radii ($R_{\rm{NIR}}$) with stellar half-mass radii (\rmass) derived with multi-color light profiles from CANDELS HST imaging. In general agreement with previous work, we find that $R_{\rm{NIR}}$ and \rmass~are up to 40\%~smaller than the rest-frame optical half-light radius $R_{\rm{opt}}$. The agreement between $R_{\rm{NIR}}$ and \rmass~is excellent, with negligible systematic offset ($<$0.03 dex) up to $z=2$ for quiescent galaxies and up to $z=1.5$ for star-forming galaxies. We also deproject the profiles to estimate \rmassd, the radius of a sphere containing 50\% of the stellar mass. We present the $R-M_\star$ distribution of galaxies at $0.5<z<1.5$, comparing $R_{\rm{opt}}$, \rmass~and \rmassd. The slope is significantly flatter for \rmass~and \rmassd~ compared to $R_{\rm{opt}}$, mostly due to downward shifts in size for massive star-forming galaxies, while \rmass~and \rmassd~do not show markedly different trends. Finally, we show rapid size evolution ($R\propto (1+z)^{-1.7\pm0.1}$) for massive ($M_\star>10^{11}~M_\odot$) quiescent galaxies between $z=0.5$ and $z=2.3$, again comparing $R_{\rm{opt}}$, \rmass~and \rmassd. We conclude that the main tenets of the size evolution narrative established over the past 20 years, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR.Comment: Submitted to ApJ. Comments welcom