Star Formation in Emission-Line Galaxies Between Redshifts of 0.8 and 1.6

Optical spectra of 14 emission-line galaxies representative of the 1999 NICMOS parallel grism Ha survey of McCarthy et al. are presented. Of the 14, 9 have emission lines confirming the redshifts found in the grism survey. The higher resolution of our optical spectra improves the redshift accuracy by a factor of 5. The [O II]/Ha values of our sample are found to be more than two times lower than expected from Jansen et al. This [O II]/Ha ratio discrepancy is most likely explained by additional reddening in our Ha-selected sample [on average, as much as an extra E(B-V) = 0.6], as well as to a possible stronger dependence of the [O II]/Ha ratio on galaxy luminosity than is found in local galaxies. The result is that star formation rates (SFRs) calculated from [O II]3727 emission, uncorrected for extinction, are found to be on average 4 +/- 2 times lower than the SFRs calculated from Ha emission. Classification of emission-line galaxies as starburst or Seyfert galaxies based on comparison of the ratios [O II]/Hb and [Ne III]3869/Hb is discussed. New Seyfert 1 diagnostics using the Ha line luminosity, H-band absolute magnitude, and Ha equivalent widths are also presented. One galaxy is classified as a Seyfert 1 based on its broad emission lines, implying a comoving number density for Seyfert 1s of 2.5{+5.9, -2.1} times 10^{-5} Mpc^{-3}. This commoving number density is a factor of 2.4{+5.5,-2.0} times higher than estimated by other surveys.Comment: 51 pages, 18 figures; Accepted for publication in the Astrophysical Journal; Revised version with minor changes and an additional reference which gives further support to our conclusion

Abundance Profiles and Kinematics of Damped Lyman-alpha Absorbing Galaxies at z < 0.65

We present a spectroscopic study of six damped Lya absorption (DLA) systems at z<0.65, based on moderate-to-high resolution spectra of the galaxies responsible for the absorbers. Combining known metallicity measurements of the absorbers with known optical properties of the absorbing galaxies, we confirm that the low metal content of the DLA population can arise naturally as a combination of gas cross-section selection and metallicity gradients commonly observed in local disk galaxies. We also study the Tully-Fisher relation of the DLA-selected galaxies and find little detectable evidence for evolution in the disk population between z=0 and z~0.5. Additional results of our analysis are as follows. (1) The DLA galaxies exhibit a range of spectral properties, from post-starburst, to normal disks, and to starburst systems, supporting the idea that DLA galaxies are drawn from the typical field population. (2) Large rotating HI disks of radius 30 h^{-1} kpc and of dynamic mass M_dyn > 10^{11} h^{-1} M_sun appear to be common at intermediate redshifts. (3) Using an ensemble of six galaxy-DLA pairs, we derive an abundance profile that is characterized by a radial gradient of -0.041 +/- 0.012 dex per kiloparsec (or equivalently a scale length of 10.6 h^{-1} kpc) from galactic center to 30 h^{-1} kpc radius. (4) Adopting known N(HI) profiles of nearby galaxies and the best-fit radial gradient, we further derive an N(HI)-weighted mean metallicity _weighted = -0.50 +/- 0.07 for the DLA population over 100 random lines of sight, consistent with _weighted = -0.64 (-0.86, +0.40) observed for z~1 DLA systems from Prochaska et al. Our analysis demonstrates that the low metal content of DLA systems does not rule out the possibility that the DLA population trace the field galaxy population.Comment: 57 pages, 17 figures, to appear in the ApJ 20 February 2005 issue; a pdf version of the paper with full-resolution figures is available at http://falcon.mit.edu/~hchen/public/tmp/dlachem.pd

To Extend or not to Extend: on the Uniqueness of Browser Extensions and Web Logins

Recent works showed that websites can detect browser extensions that users install and websites they are logged into. This poses significant privacy risks, since extensions and Web logins that reflect user's behavior, can be used to uniquely identify users on the Web. This paper reports on the first large-scale behavioral uniqueness study based on 16,393 users who visited our website. We test and detect the presence of 16,743 Chrome extensions, covering 28% of all free Chrome extensions. We also detect whether the user is connected to 60 different websites. We analyze how unique users are based on their behavior, and find out that 54.86% of users that have installed at least one detectable extension are unique; 19.53% of users are unique among those who have logged into one or more detectable websites; and 89.23% are unique among users with at least one extension and one login. We use an advanced fingerprinting algorithm and show that it is possible to identify a user in less than 625 milliseconds by selecting the most unique combinations of extensions. Because privacy extensions contribute to the uniqueness of users, we study the trade-off between the amount of trackers blocked by such extensions and how unique the users of these extensions are. We have found that privacy extensions should be considered more useful than harmful. The paper concludes with possible countermeasures.Comment: accepted at WPES 201

A New Look At Carbon Abundances In Planetary Nebulae. III. DDDM1, IC 3568, IC4593, NGC 6210, NGC 6720, NGC 6826, & NGC 7009

This paper is the third in a series reporting on a study of carbon abundances in a carefully chosen sample of planetary nebulae representing a large range in progenitor mass and metallicity. We make use of the IUE Final Archive database containing consistently-reduced spectra to measure line strengths of C III] 1909 along with numerous other UV lines for the planetary nebulae DDDM1, IC 3568, IC 4593, NGC 6210, NGC 6720, NGC 6826, & NGC 7009. We combine the IUE data with line strengths from optical spectra obtained specifically to match the IUE slit positions as closely as possible, to determine values for the abundance ratios He/H, O/H, C/O, N/O, and Ne/O. The ratio of C III] 1909/C II 4267 is found to be effective for merging UV and optical spectra when He II 1640/4686 is unavailable. Our abundance determination method includes a 5-level program whose results are fine-tuned by corrections derived from detailed photoionization models constrained by the same set of emission lines. All objects appear to have subsolar levels of O/H, and all but one show N/O levels above solar. In addition, the seven planetary nebulae span a broad range in C/O values. We infer that many of our objects are matter bounded, and thus the standard ionization correction factor for N/O may be inappropriate for these PNe. Finally, we estimate C/O using both collisionally-excited and recombination lines associated with C+2 and find the well established result that abundances from recombination lines usually exceed those from collisionally-excited lines by several times.Comment: 36 pages, 7 tables, 2 figures, latex. Tables and figures supplied as two separate postscript files. Accepted for publication in Ap

IN VITRO EQUIVALENCE STUDY OF GENERIC METFORMIN HYDROCHLORIDE TABLETS UNDER BIOWAIVER CONDITIONS

Background: Generic drugs are smarter alternative to expensive brands, it is bio- equivalent formula of any branded drug. FDA approved that generic drugs are the safest to consume, the medicines meet the similar manufacturing standards followed while producing an innovator drug, however, the color, shape, taste and packaging of generics is different from the innovator product. In short, a generic drug should be bioequivalent to its brand counterpart. Metformin was initially marketed under the name of Glucophage®, and now the market is loaded by generics of different origin, and price variability. Method: Our study was conducted to determine whether metformin generics are bioequivalent to the innovator drug Glucophage®. In-vitro bioequivalence testing under Biowaiver conditions can predict bioequivalence in a safe, fast, and less expensive method. Thus, study was performed on Metformin tablets to assess whether generics are bioequivalent to the innovator and hence be interchangeable. Results: The quality control results of the thickness, hardness, friability, disintegration, weight uniformity, content uniformity, and assay showed that most metformin tablets complied with the USP 34 NF29 2011 specifications. Dissolution testing under biowaiver conditions showed different results. All tablets of the generics and innovator Glucophage® were able to dissolve by more than 85% within 15 min. Two generics were bioequivalent to the innovator Glucophage® having f2≥ 50 in the three dissolution media. The rest of generics showed variable results. Conclusion: Generics of metformin varied in their bioequivalency to the innovator Gluocophage®. This variation could be explained by different excipients, and manufacturing conditions. In-vivo bioequivalence testing should be conducted to confirm that the innovator could be safely interchangeable with the brand and this variation won’t affect the safety and efficacy of the drug

Interpreting a Diagnosis of Atypical Squamous Cells of Undetermined Significance in Cervical Cytology and its Association with Human Papillomavirus: A retrospective analysis of 180 cases in Kuwait

Objectives: Atypical squamous cells of undetermined significance (ASC-US) represent a diagnostic challenge during cervical cytology. This study aimed to review and identify high-risk human papillomavirus (HR-HPV) genotypes among previously diagnosed ASC-US cases in Kuwait. Methods: This retrospective study analysed 180 cases diagnosed as ASC-US between June 2017 and May 2018 at the Mubarak Al-Kabeer Hospital, Kuwait. Cervical specimens were assayed to determine the presence of HR-HPV DNA; subsequently, positive cases underwent genotyping and were categorised into three groups (HPV 16, HPV 18/45 and other HR-HPV types). Results: In total, ASC-US was confirmed in only 105 cases (58.3%), with the remaining cases reclassified as negative for intraepithelial lesions or malignancy (NILM; 32.2%) and epithelial cell abnormalities (ECA; 9.4%). Of these, HRHPV DNA was present in 20 ASC-US (19%), one NILM (1.7%) and six ECA (35.3%) cases. There were 62 Kuwaiti and 43 non-Kuwaiti women with confirmed ASC-US; of these, three (4.8%), six (9.7%) and four (6.5%) Kuwaitis and one (2.3%), one (2.3%) and five (11.6%) non-Kuwaitis had HPV 16, both HPV 16 and 18/45 and other HRHPV genotypes, respectively. Of those with HR-HPV DNA, the NILM case had the HPV 18/45 genotype, while the six ECA cases had the HPV 16 (n = 1), both HPV 16 and 18/45 (n = 1) and other HR-HPV (n = 4) genotypes. Conclusion: Overall, HR-HPV DNA was present in 19% of ASC-US cases compared to 1.7% of NILM cases initially misdiagnosed as ASC-US. Re-review of cervical cytology diagnoses may reduce unnecessary costs associated with HR-HPV genotyping. Keywords: Cervical Smears; Atypical Squamous Cells of Undetermined Significance; Human Papilloma Virus; Cytological Techniques; Papanicolaou Test; Kuwait

Star Formation and X-ray Emission in Distant Star Forming Galaxies

About 45% of the point sources detected in the 2 Ms Chandra exposure of the HDF-N can be matched with moderately bright galaxies with z<1.4 that have been studied by the Caltech Faint Galaxy Redshift Survey. Although the optical spectra of these galaxies appear normal, based on their X-ray properties ~20% of them appear to contain weak AGNs. More than 90% of the X-ray photons detected by Chandra from galaxies within the redshift regime 0.4 < z < 1.1 are powered by accretion onto massive black holes. For the sample of galaxies in common, we use their emitted luminosity in the 3727 A line of [OII] to estimate their star formation rate (SFR). The X-ray emitting galaxies are not those with the highest rest frame equivalent width in this emission line, but rather are among those with the highest SFR. With SFR corrected for inclination effects, the distant galaxies show a L(X) -- SFR relationship that is comparable to that of local galaxies. The HDF sample has a significantly higher median SFR and median SFR/galaxy stellar mass than does a sample of local star forming galaxies. We demonstrate that the observed SFR for most of the galaxies at z~1 in the HDF sample, if maintained as constant over their ages, suffices to produce the stellar mass observed in these galaxies. A rise in SFR at still earlier times is not required. We provide further evidence to support the conclusion that, once AGNs are eliminated, X-ray emission in these distantstar forming galaxies is related to the SFR through the same physical mechanisms that prevail locally.Comment: Accepted for the Astrophysical Journa

Consideration for Scaffolding Open-Ended Engineering Problems: Instructor Reflections After Three Years

This full research-to-practice paper is a collaboration between researchers and instructors to examine the scaffolding of open-ended problems. Most assigned homework problems are closed-ended with one correct answer and are unlike the ill-defined problems practicing engineers solve in the workplace. To begin bridging this gap, our research team of engineering education researchers and instructors have been designing and implementing ill-defined, open-ended homework problems for the past three years. This study presents instructor reflections on considerations for scaffolding open-ended problems, made after examining survey data from their own students. We present the results in six practices of scaffolding that better support students in their solving of the problems

Recombination Line vs. Forbidden Line Abundances in Planetary Nebulae

Recombination lines (RLs) of C II, N II, and O II in planetary nebulae (PNs) have been found to give abundances that are much larger in some cases than abundances from collisionally-excited forbidden lines (CELs). The origins of this abundance discrepancy are highly debated. We present new spectroscopic observations of O II and C II recombination lines for six planetary nebulae. With these data we compare the abundances derived from the optical recombination lines with those determined from collisionally-excited lines. Combining our new data with published results on RLs in other PNs, we examine the discrepancy in abundances derived from RLs and CELs. We find that there is a wide range in the measured abundance discrepancy Delta(O+2) = log O+2(RL) - log O+2(CEL), ranging from approximately 0.1 dex up to 1.4 dex. Most RLs yield similar abundances, with the notable exception of O II multiplet V15, known to arise primarily from dielectronic recombination, which gives abundances averaging 0.6 dex higher than other O II RLs. We compare Delta(O+2) against a variety of physical properties of the PNs to look for clues as to the mechanism responsible for the abundance discrepancy. The strongest correlations are found with the nebula diameter and the Balmer surface brightness. An inverse correlation of Delta(O+2) with nebular density is also seen. Similar results are found for carbon in comparing C II RL abundances with ultraviolet measurements of C III].Comment: 48 pages, 14 figures, accepted for publication in the Astrophysical Journal Supplemen