Search

The growing number of multi-epoch optical and infrared sky surveys are uncovering unprecedented numbers of new variable stars, of an increasing number of types. The short interval between observations in adjacent near infrared filters in the UKIDSS Galactic Plane Survey (UGPS) allows for the discovery of variability on the timescale of minutes. We report on the nature of one such object, through the use of optical spectroscopy, time-series photometry and targeted X-ray observations. We propose that UGPS J194310.32+183851.8 is a magnetic cataclysmic variable star of novel character, probably featuring a longer than average spin period and an orbital period likely to be shorter than the period gap (i.e. P$_{\text{orb}}$, 9 pages, 9 figures

We present a new method to derive binary inclinations in quiescent black hole (BH) X-ray transients (XRTs), based on the depth of the trough (T) from double-peaked Ha emission profiles arising in accretion discs. We find that the inclination angle (i) is linearly correlated with T in phase-averaged spectra with sufficient orbital coverage (>~50 per cent) and spectral resolution, following i (deg)=93.5 x T +23.7. The correlation is caused by a combination of line opacity and local broadening, where a leading (excess broadening) component scales with the de-projected velocity of the outer disc. Interestingly, such scaling allows to estimate the fundamental ratio M1/Porb by simply resolving the intrinsic width of the double-peak profile. We apply the T-i correlation to derive binary inclinations for GRO J0422+32 and Swift J1357-0933, two BH XRTs where strong flickering activity has hindered determining their values through ellipsoidal fits to photometric light curves. Remarkably, the inclination derived for GRO J0422+32 (i=55.6+-4.1) implies a BH mass of 2.7+0.7-0.5 Msun thus placing it within the gap that separates BHs from neutron stars. This result proves that low-mass BHs exist in nature and strongly suggests that the so-called "mass gap" is mainly produced by low number statistics and possibly observational biases. On the other hand, we find that Swift J1357-0933 contains a 10.9+1.7-1.6 Msun BH seen nearly edge on (i=87.4+2.6-5.6 deg). Such extreme inclination, however, should be treated with caution since it relies on extrapolating the T-i correlation beyond i>~75 deg, where it has not yet been tested., Accepted for publication in MNRAS, 21 pages, 15 figures, 6 Tables; references and typos corrected

The All-Sky Automated Survey for Supernovae (ASAS-SN) provides long baseline (${\sim}4$ yrs) light curves for sources brighter than V$\lesssim17$ mag across the whole sky. The Transiting Exoplanet Survey Satellite (TESS) has started to produce high-quality light curves with a baseline of at least 27 days, eventually for most of the sky. The combination of ASAS-SN and TESS light curves probes both long and short term variability in great detail, especially towards the TESS continuous viewing zones (CVZ) at the ecliptic poles. We have produced ${\sim}1.3$ million V-band light curves covering a total of ${\sim}1000 \, \rm deg^2$ towards the southern TESS CVZ and have systematically searched these sources for variability. We have identified ${\sim} 11,700$ variables, including ${\sim} 7,000$ new discoveries. The light curves and characteristics of the variables are all available through the ASAS-SN variable stars database (https://asas-sn.osu.edu/variables). We also introduce an online resource to obtain pre-computed ASAS-SN V-band light curves (https://asas-sn.osu.edu/photometry) starting with the light curves of the ${\sim}1.3$ million sources studied in this work. This effort will be extended to provide ASAS-SN light curves for ${\sim}50\;$million sources over the entire sky., Comment: 13 pages, 12 figures. Accepted by MNRAS

The variable stars in the VSX catalog are derived from a multitude of inhomogeneous data sources and classification tools. This inhomogeneity complicates our understanding of variable star types, statistics, and properties, and it directly affects attempts to build training sets for current (and next) generation all-sky, time-domain surveys. We homogeneously analyze the ASAS-SN V-band light curves of ${\sim}412,000$ variables from the VSX catalog. The variables are classified using an updated random forest classifier with an $F_1$ score of 99.4\% and refinement criteria for individual classifications. We have derived periods for ${\sim}52,000$ variables in the VSX catalog that lack a period, and have reclassified ${\sim} 17,000$ sources into new broad variability groups with high confidence. We have also reclassified ${\sim} 94,000$ known variables with miscellaneous/generic classifications. The light curves, classifications, and a range of properties of the variables are all available through the ASAS-SN variable stars database (https://asas-sn.osu.edu/variables). We also include the V-band light curves for a set of ${\sim}4,000$ rare variables and transient sources, including cataclysmic variables, symbiotic binaries and flare stars., Comment: 37 pages, 42 figures, 11 tables. Accepted by MNRAS. The catalog of variable stars and the V-band light curves are available from the ASAS-SN Variable Stars Database at https://asas-sn.osu.edu/variables

We explore the synergy between photometric and spectroscopic surveys by searching for periodic variable stars among the targets observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) using photometry from the All-Sky Automated Survey for Supernovae (ASAS-SN). We identified 1924 periodic variables among more than 258000 APOGEE targets; 465 are new discoveries. We homogeneously classified 430 eclipsing and ellipsoidal binaries, 139 classical pulsators (Cepheids, RR Lyrae and delta Scuti), 719 long period variables (pulsating red giants) and 636 rotational variables. The search was performed using both visual inspection and machine learning techniques. The light curves were also modeled with the damped random walk stochastic process. We find that the median [Fe/H] of variable objects is lower by 0.3 dex than that of the overall APOGEE sample. Eclipsing binaries and ellipsoidal variables are shifted to a lower median [Fe/H] by 0.2 dex. Eclipsing binaries and rotational variables exhibit significantly broader spectral lines than the rest of the sample. We make ASAS-SN light curves for all the APOGEE stars publicly available and provide parameters for the variable objects., Comment: accepted to MNRAS

The All-Sky Automated Survey for Supernovae (ASAS-SN) is the first optical survey to routinely monitor the whole sky with a cadence of $\sim2-3$ days down to V$\lesssim17$ mag. ASAS-SN has monitored the whole sky since 2014, collecting $\sim100-500$ epochs of observations per field. The V-band light curves for candidate variables identified during the search for supernovae are classified using a random forest classifier and visually verified. We present a catalog of 66,179 bright, new variable stars discovered during our search for supernovae, including 27,479 periodic variables and 38,700 irregular variables. V-band light curves for the ASAS-SN variables are available through the ASAS-SN variable stars database (https://asas-sn.osu.edu/variables). The database will begin to include the light curves of known variable stars in the near future along with the results for a systematic, all-sky variability survey., 21 pages, 19 figures, 5 tables. Accepted for publication in MNRAS. The catalog of variable stars and the V-band light curves are available from the ASAS-SN Variable Stars Database at https://asas-sn.osu.edu/variables

We present a catalog of 4880 newly identified RR Lyrae variable stars (4433 RRab, 446 RRc and 1 RRd) found during the search for supernovae by the All-Sky Automated Survey for Supernovae (ASAS-SN). The light curves, classified using the "Upsilon" random forest classifier and visually verified, are available through the ASAS-SN variable star database (https://asas-sn.osu.edu/variables). The database also contains light curves for an expanding number of additional new variables (~50,000 at present) and will begin to include the light curves of known variable stars in the near future., Comment: 3 pages, 1 figure. The ASAS-SN Variable Star Database is available online at https://asas-sn.osu.edu/variables

The All-Sky Automated Survey for Supernovae (ASAS-SN) is working towards imaging the entire visible sky every night to a depth of V~17 mag. The present data covers the sky and spans ~2-5~years with ~100-400 epochs of observation. The data should contain some ~1 million variable sources, and the ultimate goal is to have a database of these observations publicly accessible. We describe here a first step, a simple but unprecedented web interface https://asas-sn.osu.edu/ that provides an up to date aperture photometry light curve for any user-selected sky coordinate. Because the light curves are produced in real time, this web tool is relatively slow and can only be used for small samples of objects. However, it also imposes no selection bias on the part of the ASAS-SN team, allowing the user to obtain a light curve for any point on the celestial sphere. We present the tool, describe its capabilities, limitations, and known issues, and provide a few illustrative examples., 8 pages, 9 figures, submitted to PASP

We present the identification of optical counterparts to 23 GBS X-ray sources. All sources are classified as accreting binaries according to the emission-line characteristics inferred from medium-resolution spectroscopy. To distinguish accreting binaries from chromospherically active objects, we develop criteria based on Hα and He I λλ5786, 6678 emission-line properties available in the literature. The spectroscopic properties and photometric variability of each object is discussed and a classification is given where possible. At least 12 of the 23 systems show an accretion-dominated optical spectrum and another 6 show stellar absorption features in addition to emission lines indicating that they are probably accreting binaries in quiescence or in a low accretion rate state. Two sources are confirmed to be eclipsing: CX207 and CX794. CX207 is likely a magnetic cataclysmic variable (CV), while CX794 is a nova-like CV in the period gap. Finally, the large broadening (2100 km s-1 FWHM) of the Hα emission lines in CX446 and CX1004 suggests that they are also high-inclination or even eclipsing systems. Whether the compact object is a white dwarf in an eclipsing CV, a neutron star or a black hole in a high-inclination low-mass X-ray binary remains to be established. 27 pages, 7 figures, 2 tables, submitted to MNRAS ispartof: Monthly Notices of the Royal Astronomical Society vol:440 issue:1 pages:365-386 status: published

We report on the near-infrared matches, drawn from three surveys, to the 1640 unique X-ray sources detected by Chandra in the Galactic Bulge Survey (GBS). This survey targets faint X-ray sources in the Bulge, with a particular focus on accreting compact objects. We present all viable counterpart candidates and associate a false alarm probability (FAP) to each near-infrared match in order to identify the most likely counterparts. The false alarm probability takes into account a statistical study involving a chance alignment test, as well as considering the positional accuracy of the individual X-ray sources. We find that although the star density in the Bulge is very high, ~90% of our sources have a false alarm probability < 10%, indicating that for most X-ray sources, viable near-infrared counterparts candidates can be identified. In addition to the FAP, we provide positional and photometric information for candidate counterparts to ~95% of the GBS X-ray sources. This information in combination with optical photometry, spectroscopy and variability constraints will be crucial to characterize and classify secure counterparts., 16 pages, 14 figures, accepted for publication in MNRAS, full version of final Table (4) will be available online through MNRAS and CDS

As part of the Chandra Galactic Bulge Survey (GBS), we present a catalogue of optical sources in the GBS footprint. This consists of two regions centered at Galactic latitude b = 1.5 degrees above and below the Galactic Centre, spanning (l x b) = (6x1) degrees. The catalogue consists of 2 or more epochs of observations for each line of sight in r', i' and H{\alpha} filters. It is complete down to r' = 20.2 and i' = 19.2 mag; the mean 5{\sigma} depth is r' = 22.5 and i' = 21.1 mag. The mean root-mean-square residuals of the astrometric solutions is 0.04 arcsec. We cross-correlate this optical catalogue with the 1640 unique X-ray sources detected in Chandra observations of the GBS area, and find candidate optical counterparts to 1480 X-ray sources. We use a false alarm probability analysis to estimate the contamination by interlopers, and expect ~ 10 per cent of optical counterparts to be chance alignments. To determine the most likely counterpart for each X-ray source, we compute the likelihood ratio for all optical sources within the 4{\sigma} X-ray error circle. This analysis yields 1480 potential counterparts (~ 90 per cent of the sample). 584 counterparts have saturated photometry (r', Comment: 18 pages, 18 figures. Published in MNRAS. 2016MNRAS.458.4530W

The din of the Hali‘imaile lunch crowd drifted to the veranda where Bob and Evelyn sat enjoying the breeze. “The pineapple upside-down cake I just had for dessert is the best way to eat pineapple I've ever found,” Bob said. “I'll see if I can get the recipe off the restaurant's Web site. Are you ready to go?” Evelyn asked. Bob preferred returning to the condo in Kihei to searching the north shore of Maui for some place he had no desire to visit. “Are you sure you want to go out there?” “Yes! I promised Dr. Winthrop. Anyway, it's just out of Pā'ia. We'll get back in plenty of time for you to sit on the lanai and read neurology journals.” “You know I have to get caught up on vacations,” Bob mumbled. They walked to the rented Chevrolet Impala. Bob slid behind the wheel and said, “This is something—early January, the car's been sitting outside, and you have to turn on the air conditioning to cool it off!” “It's not Minneapolis, for sure. I love seeing everything so green,” Evelyn said. Bob pulled out of the gravel parking lot and drove cautiously on the narrow, winding road. In the wind the sugarcane in the fields on each side undulated in broad waves, motion vivid in Bob's mind, the inland correlate of that lapping the island's shores. The road intersected Baldwin Avenue, which he took into Pā'ia. “Go slow,” Evelyn requested. “Let's pick up flowers here, and I'll get the directions then.” When they didn't pass a flower shop, Bob thought, ‘The whole purpose is taking flowers, and we're going to get out there without any.' Once past …

Reaching for the carafe, Lynn asked, “Would you like more coffee?” Sitting at the breakfast table, John continued to look out the glass patio slider and did not answer. The leaf-withering chill of late autumn had weathered the landscape. Lynn finished rinsing the dishes. After draping the dishrag over the spout, she asked, “Did you take your morning pills?” “Yeah, I took 'em,” John said. “I'm going to work in the church office this morning,” Lynn said. “Then I'll pick up groceries for your mother. I'll be back home after I drop them by and fix her some lunch.” “I'm taking the cell phone with me,” Lynn said. “You'll call me if the pager goes off?” Expressionless and still staring outside, John mumbled, “We'll see.” “You'll call?” she asked again. “All right!” John shouted. “I'll call you before the pager stops beeping!” Tense and tearful, Lynn hurried from the room. John heard the car start and pull away. He did not leave the table or shift his gaze. \* * *| \* * *| * * “Transplant Office, Beth Sawyer, Coordinator,” came the voice over the phone. “Oh, Beth, this is Lynn Ellis. I'm calling you about John. He's not right. He's never been like this. He's angry, depressed, won't talk …” “Lynn, emotional reactions are common at this stage, leaving the hospital after a severe illness. Waiting for a heart transplant is stressful.” “He'll carry the pager for the call to come right in for the surgery, but …” Crying, Lynn said, “I'm afraid he's not going to go through with it!” Beth gave Lynn a moment to compose herself, then said, “I see.” She paused before continuing. “John's due for his 1-month check-up next week. The …

Acute necrotizing fasciitis is a rare but frequently catastrophic infection of the subcutaneous tissues and fascial sheaths. It is rare in infants and children. The case of a 3 1/2-year-old boy with acute necrotizing fasciitis caused by group A beta hemolytic streptococcus is described.

“9–1-1.” “My husband's dead! My son just found him!” “What's your name, M'am?” “Out in the barn, he's dead!” “M'am, what's your name?” When the woman did not answer, the dispatcher called, “M'am, M'am!” Then he heard a young man's voice. “Let me have your phone, Mom. Here! Let me talk to them.” \* * *| \* * *| \* * *| Buster's cell phone rang out its melody. Centered on one side of its leather case was a silver star surrounded by a circle touching each of the 7 points. The tall man flipped the phone open, held it to his ear, and said, “Sheriff Holman.” “Buster, this is Aubrey. We got a suicide out in Cougar Gulch. This guy suffocated himself, plastic bag over the head. His son found him out in his barn a couple of hours ago.” “Was there a note?” Buster asked. “We haven't found one. Hank's in the house with the boy now, goin' through his things. But the wife said he was just diagnosed with cancer. His father and uncle had the same thing. The uncle was the guy that jumped off the bridge over Wolf Lodge Bay 'bout 15 years ago. You 'member that case?” “I remember,” Buster said. “Has the M.E. been there yet?” “Doc's about to finish, but I won't let 'em move the body 'til you get here. You gotta see this one!” “I can be right out there,” Buster said. Aubrey continued, “Can you imagine the poor kid walkin' into that barn?” “What's the address?” Buster asked, not wanting to go into the family's anguish with Aubrey. Buster had to do the job, had to and would do it, as ugly as this part of it always was. \* * *| \* * *| \* * *| Janice …

The rate of removal of various fatty compounds from a variety of textile fibres has been studied by means of a radioactive-tracer technique. The effect of the nature of the detergent solution and of the age of the soiling has been examined. The results have been compared with those obtained by reflectance measurements.

The widths of the J=1 to 2 transition of OCS broadened by collisions with OCS and with CHF3 and the J=0 to 1 transition CHF3 broadened by collisions with CHF3 and with OCS have been measured by a digital fitting of the recorded line shape to the theoretical line shape function. Present theory of rotation energy transfer accurately predicts the width of the self-broadened CHF3 line and the two foreign gas broadening cases, but there is a small but apparently real discrepancy in the case of the OCS self-broadening.

Ridged rows and winter cover crops were used to control erosion and promote good tilth in 1-year tobacco rotations. Studies conducted over a 5-year period comparing flat cultivation versus ridged rows showed that tobacco yields were increased substantially by ridging in wet years. In dry years, yields on ridged and flat plots were essentially the same. Winter cover crops and their management affected both the yield and quality of the succeeding tobacco crop. Ryegrass alone reduced yield and vetch alone lowered quality. Highest yields and quality of tobacco followed mixed cover crops of rye and vetch or ryegrass and vetch. Late turning of the mixed cover crops was better than early turning. Aside from supplying more organic residues to the soil, late turning promoted the larger yield of tobacco, of as good a quality as early turning.

The All-Sky Automated Survey for Supernovae (ASAS-SN) provides long baseline (${\sim}4$ yrs) light curves for sources brighter than V$\lesssim17$ mag across the whole sky. As part of our effort to characterize the variability of all the stellar sources visible in ASAS-SN, we have produced ${\sim}30.1$ million V-band light curves for sources in the southern hemisphere using the APASS DR9 catalog as our input source list. We have systematically searched these sources for variability using a pipeline based on random forest classifiers. We have identified ${\sim} 220,000$ variables, including ${\sim} 88,300$ new discoveries. In particular, we have discovered ${\sim}48,000$ red pulsating variables, ${\sim}23,000$ eclipsing binaries, ${\sim}2,200$ $\delta$-Scuti variables and ${\sim}10,200$ rotational variables. The light curves and characteristics of the variables are all available through the ASAS-SN variable stars database (https://asas-sn.osu.edu/variables). The pre-computed ASAS-SN V-band light curves for all the ${\sim}30.1$ million sources are available through the ASAS-SN photometry database (https://asas-sn.osu.edu/photometry). This effort will be extended to provide ASAS-SN light curves for sources in the northern hemisphere and for V$\lesssim17$ mag sources across the whole sky that are not included in APASS DR9., Comment: 17 pages, 14 figures. Accepted by MNRAS

IN the course of investigations into detergency using radioactive isotopes, some interesting observations have been made. The chopped fibre technique1 was used, and the cotton fibre was soiled as described previously2, but with a proportion of the stearic acid replaced by stearic acid-1-14C. The rate of removal of stearic acid from the fibre after washing with different detergent solutions for various times was measured by the residual activity of the fibre compared with the initial activity of the unwashed fibre. The fibre was made into smooth pads and activities were determined by an end-window counter.