This paper describes the organization of the database and the catalog data products from the Pan-STARRS1 3 π Steradian Survey. The catalog data products are available in the form of an SQL-based relational database from MAST, the Mikulski Archive for Space Telescopes at STScI. The database is described in detail, including the construction of the database, the provenance of the data, the schema, and how the database tables are related. Examples of queries for a range of science goals are included.

The experience of pain is different for everyone and there is considerable variability regarding pain perceptions. The recent opioid epidemic is a major source of stress for patients and clinicians alike. There is a significant need for comprehensive pain assessment and nonpharmacological treatments for pain. However, research suggests that nurses experience barriers related to the assessment and treatment of patients’ pain. Such barriers may include not having enough time to work with patients, subjective pain assessments, medication-seeking behaviors, and lack of support from treating physicians. The current study examined the perceptions of nurses regarding barriers to pain assessment, documentation, and treatments in a midwestern hospital system. A survey monkey questionnaire was sent to nurses working in hospital units (N=111) and regional clinics (N=29). Results suggest that nurses in both hospital and clinic settings are willing to recommend certain non-pharmacologic interventions (e.g., relaxation, stretching) for pain management. Hospital nurses are willing to administer non-pharmacologic interventions at a much higher rate compared to their clinic counterparts. The most frequently cited barrier to assessing pain was a disconnect between patients’ self-report of pain and nurses assessment of patients’ pain behavior. Nurses requested several trainings to enhance competency for overall pain management including education regarding medication-seeking behavior, functional or objective pain assessment, and cognitive and behavioral interventions for pain management. The results of the current study will be used to create an educational program that will be developed and administered to allied health professionals to increase awareness of assessing and managing pain from a more holistic perspective. Additionally, a new pain management model will be proposed that incorporates patients’ self-report of pain, biopsychosocial factors, objective assessment information, and clinical factors. (Topolovec-Vranic, American Journal of Clinical Care, 2017; Winslow, The American Journal of Nursing, 1998). The experience of pain is different for everyone and there is considerable variability regarding pain perceptions. The recent opioid epidemic is a major source of stress for patients and clinicians alike. There is a significant need for comprehensive pain assessment and nonpharmacological treatments for pain. However, research suggests that nurses experience barriers related to the assessment and treatment of patients’ pain. Such barriers may include not having enough time to work with patients, subjective pain assessments, medication-seeking behaviors, and lack of support from treating physicians. The current study examined the perceptions of nurses regarding barriers to pain assessment, documentation, and treatments in a midwestern hospital system. A survey monkey questionnaire was sent to nurses working in hospital units (N=111) and regional clinics (N=29). Results suggest that nurses in both hospital and clinic settings are willing to recommend certain non-pharmacologic interventions (e.g., relaxation, stretching) for pain management. Hospital nurses are willing to administer non-pharmacologic interventions at a much higher rate compared to their clinic counterparts. The most frequently cited barrier to assessing pain was a disconnect between patients’ self-report of pain and nurses assessment of patients’ pain behavior. Nurses requested several trainings to enhance competency for overall pain management including education regarding medication-seeking behavior, functional or objective pain assessment, and cognitive and behavioral interventions for pain management. The results of the current study will be used to create an educational program that will be developed and administered to allied health professionals to increase awareness of assessing and managing pain from a more holistic perspective. Additionally, a new pain management model will be proposed that incorporates patients’ self-report of pain, biopsychosocial factors, objective assessment information, and clinical factors. (Topolovec-Vranic, American Journal of Clinical Care, 2017; Winslow, The American Journal of Nursing, 1998).

Author(s): Chambers, KC; Magnier, EA; Metcalfe, N; Flewelling, HA; Huber, ME; Waters, CZ; Denneau, L; Draper, PW; Farrow, D; Finkbeiner, DP; Holmberg, C; Koppenhoefer, J; Price, PA; Rest, A; Saglia, RP; Schlafly, EF; Smartt, SJ; Sweeney, W; Wainscoat, RJ; Burgett, WS; Chastel, S; Grav, T; Heasley, JN; Hodapp, KW; Jedicke, R; Kaiser, N; Kudritzki, R-P; Luppino, GA; Lupton, RH; Monet, DG; Morgan, JS; Onaka, PM; Shiao, B; Stubbs, CW; Tonry, JL; White, R; Banados, E; Bell, EF; Bender, R; Bernard, EJ; Boegner, M; Boffi, F; Botticella, MT; Calamida, A; Casertano, S; Chen, W-P; Chen, X; Cole, S; Deacon, N; Frenk, C; Fitzsimmons, A; Gezari, S; Gibbs, V; Goessl, C; Goggia, T; Gourgue, R; Goldman, B; Grant, P; Grebel, EK; Hambly, NC; Hasinger, G; Heavens, AF; Heckman, TM; Henderson, R; Henning, T; Holman, M; Hopp, U; Ip, W-H; Isani, S; Jackson, M; Keyes, CD; Koekemoer, AM; Kotak, R; Le, D; Liska, D; Long, KS; Lucey, JR; Liu, M; Martin, NF; Masci, G; McLean, B; Mindel, E; Misra, P; Morganson, E; Murphy, DNA | Abstract: Pan-STARRS1 has carried out a set of distinct synoptic imaging sky surveys including the $3\pi$ Steradian Survey and the Medium Deep Survey in 5 bands ($grizy_{P1}$). The mean 5$\sigma$ point source limiting sensitivities in the stacked 3$\pi$ Steradian Survey in $grizy_{P1}$ are (23.3, 23.2, 23.1, 22.3, 21.4) respectively. The upper bound on the systematic uncertainty in the photometric calibration across the sky is 7-12 millimag depending on the bandpass. The systematic uncertainty of the astrometric calibration using the Gaia frame comes from a comparison of the results with Gaia: the standard deviation of the mean and median residuals ($ \Delta ra, \Delta dec $) are (2.3, 1.7) milliarcsec, and (3.1, 4.8) milliarcsec respectively. The Pan-STARRS system and the design of the PS1 surveys are described and an overview of the resulting image and catalog data products and their basic characteristics are described together with a summary of important results. The images, reduced data products, and derived data products from the Pan-STARRS1 surveys are available to the community from the Mikulski Archive for Space Telescopes (MAST) at STScI.

Nature 502, 346–349 (2013); doi:10.1038/nature12569 In this Letter, we have identified an important error affecting Fig. 4 and Extended Data Fig. 6, as well as the values of some parameters derived from our model fits. We stress that this error in no way affects the discussion or the conclusions. Inbuilding the bolometric light curve of the superluminous supernova PTF 12dam, our code assumed that photometry from the Swift satellite was calibrated in the Vega magnitude system.

Pan-STARRS1 has carried out a set of distinct synoptic imaging sky surveys including the $3π$ Steradian Survey and the Medium Deep Survey in 5 bands ($grizy_{P1}$). The mean 5$σ$ point source limiting sensitivities in the stacked 3$π$ Steradian Survey in $grizy_{P1}$ are (23.3, 23.2, 23.1, 22.3, 21.4) respectively. The upper bound on the systematic uncertainty in the photometric calibration across the sky is 7-12 millimag depending on the bandpass. The systematic uncertainty of the astrometric calibration using the Gaia frame comes from a comparison of the results with Gaia: the standard deviation of the mean and median residuals ($ Δra, Δdec $) are (2.3, 1.7) milliarcsec, and (3.1, 4.8) milliarcsec respectively. The Pan-STARRS system and the design of the PS1 surveys are described and an overview of the resulting image and catalog data products and their basic characteristics are described together with a summary of important results. The images, reduced data products, and derived data products from the Pan-STARRS1 surveys are available to the community from the Mikulski Archive for Space Telescopes (MAST) at STScI.

The Pan-Planets survey observed an area of 42 sq deg. in the galactic disk for about 165 h. The main scientific goal of the project is the detection of transiting planets around M dwarfs. We establish an efficient procedure for determining the stellar parameters T-eff and log g of all sources using a method based on SED fitting, utilizing a three-dimensional dust map and proper motion information. In this way we identify more than 60 000 M dwarfs, which is by far the largest sample of low-mass stars observed in a transit survey to date. We present several planet candidates around M dwarfs and hotter stars that are currently being followed up. Using Monte Carlo simulations we calculate the detection efficiency of the Pan-Planets survey for different stellar and planetary populations. We expect to find 3.0(-1.6)(+3.3) hot Jupiters around F, G, and K dwarfs with periods lower than 10 days based on the planet occurrence rates derived in previous surveys. For M dwarfs, the percentage of stars with a hot Jupiter is under debate. Theoretical models expect a lower occurrence rate than for larger main sequence stars. However, radial velocity surveys find upper limits of about 1% due to their small sample, while the Kepler survey finds a occurrence rate that we estimate to be at least 0.17((+0.67)(-0.04))%, making it even higher than the determined fraction from OGLE-III for E, G and K stellar types, 0.140((+0.67)(-0.076))%. With the large sample size of Pan-Planets, we are able to determine an occurrence rate of 0.11((+0.37)(-0.02))% in case one of our candidates turns out to be a real detection. If, however, none of our candidates turn out to be true planets, we are able to put an upper limit of 0.34% with a 95% confidence on the hot Jupiter occurrence rate of M dwarfs. This limit is a significant improvement over previous estimates where the lowest limit published so far is 1.1% found in the WFCAM Transit Survey. Therefore we cannot yet confirm the theoretical prediction of a lower occurrence rate for cool stars.

The Pan-STARRS1 (PS1) survey has obtained imaging in 5 bands (grizy_P1) over 10 Medium Deep Survey (MDS) fields covering a total of 70 square degrees. This paper describes the search for apparently hostless supernovae (SNe) within the first year of PS1 MDS data with an aim of discovering new superluminous supernovae (SLSNe). A total of 249 hostless transients were discovered down to a limiting magnitude of M_AB 23.5, of which 76 were classified as Type Ia SNe. There were 57 SNe with complete light curves that are likely core-collapse SNe (CCSNe) or SLSNe and 12 of these have had spectra taken. Of these 12 hostless, non-Type Ia SNe, 7 were SLSNe of Type Ic at redshifts between 0.5-1.4. This illustrates that the discovery rate of Type Ic SLSNe can be maximised by concentrating on hostless transients and removing normal SNe Ia. We present data for two new possible SLSNe; PS1-10pm (z = 1.206) and PS1-10ahf (z = 1.1), and estimate the rate of SLSNe-Ic to be between 3^+3_-2 * 10^-5 and 8^+2_-1 * 10^-5 of the CCSNe rate within 0.3 <= z <= 1.4 by applying a Monte-Carlo technique. The rate of slowly evolving, SN2007bi-like explosions is estimated as a factor of 10 lower than this range.

We present the discovery of three new Milky Way satellites from our search for compact stellar overdensities in the photometric catalog of the Panoramic Survey Telescope and Rapid Response System 1 (Pan-STARRS 1, or PS1) 3pi survey. The first satellite, Laevens 3, is located at a heliocentric distance of d=67+/-3 kpc. With a total magnitude of Mv=-4.4+/-0.3 and a half-light radius rh=7+/-2 pc, its properties resemble those of outer halo globular clusters. The second system, Draco II/Laevens 4 (Dra II), is a closer and fainter satellite (d~20 kpc, Mv =-2.9+/-0.8), whose uncertain size (rh = 19 +8/-6 pc) renders its classification difficult without kinematic information; it could either be a faint and extended globular cluster or a faint and compact dwarf galaxy. The third satellite, Sagittarius II/Laevens 5 (Sgr II), has an ambiguous nature as it is either the most compact dwarf galaxy or the most extended globular cluster in its luminosity range (rh = 37 +9/-8 pc and Mv=-5.2+/-0.4). At a heliocentric distance of 67+/-5 kpc, this satellite lies intriguingly close to the expected location of the trailing arm of the Sagittarius stellar stream behind the Sagittarius dwarf spheroidal galaxy (Sgr dSph). If confirmed through spectroscopic follow up, this connection would locate this part of the trailing arm of the Sagittarius stellar stream that has so far gone undetected. It would further suggest that Sgr II was brought into the Milky Way halo as a satellite of the Sgr dSph.

Membership identification is the first step to determine the properties of a star cluster. Low-mass members in particular could be used to trace the dynamical history, such as mass segregation, stellar evaporation, or tidal stripping, of a star cluster in its Galactic environment. We identified member candidates with stellar masses $\sim$0.11--2.4 Msun of the intermediate-age Praesepe cluster (M44), by using Pan-STARRS and 2MASS photometry, and PPMXL proper motions. Within a sky area of 3 deg radius, 1040 candidates are identified, of which 96 are new inclusions. Using the same set of selection criteria on field stars led to an estimate of a false positive rate 16%, suggesting 872 of the candidates being true members. This most complete and reliable membership list allows us to favor the BT-Settl model in comparison with other stellar models. The cluster shows a distinct binary track above the main sequence, with a binary frequency of 20--40%, and a high occurrence rate of similar mass pairs. The mass function is consistent with that of the disk population but shows a deficit of members below 0.3 solar masses. A clear mass segregation is evidenced, with the lowest-mass members in our sample being evaporated from this disintegrating cluster.

We present grizP1 light curves of 146 spectroscopically confirmed Type Ia Supernovae (0.03 < z < 0.65) discovered during the first 1.5 years of the Pan-STARRS1 Medium Deep Survey. The Pan-STARRS1 natural photometric system is determined by a combination of on-site measurements of the instrument response function and observations of spectrophotometric standard stars. We find that the systematic uncertainties in the photometric system are currently 1.2% without accounting for the uncertainty in the HST Calspec definition of the AB system. A Hubble diagram is constructed with a subset of 113 out of 146 SNe Ia that pass our light curve quality cuts. The cosmological fit to 310 SNe Ia (113 PS1 SNe Ia + 222 light curves from 197 low-z SNe Ia), using only SNe and assuming a constant dark energy equation of state and flatness, yields w = −1.120 −0.206(Stat) +0.269 −0.291(Sys). When combined with BAO+CMB(Planck)+H0, the analysis yields ΩM = 0.280 +0.013 −0.012 and w = −1.166 +0.072 −0.069 including all identified systematics (Scolnic et al. 2013). The value of w is inconsistent with the cosmological constant value of −1 at the 2.3σ level. Tension endures after removing either the BAO or the H0 constraint, though it is strongest when including the H0 constraint. If we include WMAP9 CMB constraints instead of those from Planck, we find w = −1.124 −0.065, which diminishes the discord to < 2σ. We cannot conclude whether the tension with flat ΛCDM is a feature of dark energy, new physics, or a combination of chance and systematic errors. The full Pan-STARRS1 supernova sample with ∼3 times as many SNe should provide more conclusive results. Subject headings: supernova:general—cosmology:observations—cosmological parameters—dark energy 1 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 2 Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA 3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 4 Astronomy Department, University of Illinois at UrbanaChampaign, 1002 West Green Street, Urbana, IL 61801, USA 5 Department of Physics, University of Illinois UrbanaChampaign, 1110 W. Green Street, Urbana, IL 61801, USA 6 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 7 Department of Physics, Harvard University, 17 Oxford Street, Cambridge MA 02138 8 Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast, BT71NN, UK 9 Max Planck Institute for Astronomy, K onigstuhl 17, D69117 Heidelberg, Germany 10 Hubble Postdoctoral Fellow 11 INAF Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy 12 University of Waterloo, 200 University Ave W Waterloo, ON N2L 3G1, Canada 13 Perimeter Institute for Theoretical Physics, 31 Caroline St N, Waterloo, Ontario, N2L 2Y5, Canada 14 Department of Astronomy & Astrophysics, University of California, Santa Cruz, CA 95060, USA 20 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 15 INAF Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 16 Las Cumbres Observatory Global Telescope Network, Inc., Santa Barbara, CA 93117, USA 17 Department of Physics, University of California Santa Barbara, Santa Barbara, CA 93106-9530, USA 18 PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA. 19 Department of Physics, University of Durham Science Laboratories, South Road Durham DH1 3LE, UK ar X iv :1 31 0. 38 28 v2 [ as tr oph .C O ] 3 1 A ug 2 01 4 2 Rest, Scolnic et al.

High-redshift quasars are currently the only probes of the growth of supermassive black holes and potential tracers of structure evolution at early cosmic time. Here we present our candidate selection criteria from the Panoramic Survey Telescope & Rapid Response System 1 and follow-up strategy to discover quasars in the redshift range 5.7 < z < 6.2. With this strategy we discovered eight new 5.7 z 6.0 quasars, increasing the number of known quasars at z > 5.7 by more than 10%. We additionally recovered 18 previously known quasars. The eight quasars presented here span a large range of luminosities (-27.3 <= M-1450 <= -25.4; 19.6 21.2) and are remarkably heterogeneous in their spectral features: half of them show bright emission lines whereas the other half show a weak or no Lya emission line (25% with rest-frame equivalent width of the Lya+N v line lower than 15 A). We find a larger fraction of weak-line emission quasars than in lower redshift studies. This may imply that the weak-line quasar population at the highest redshifts could be more abundant than previously thought. However, larger samples of quasars are needed to increase the statistical significance of this finding.

We present optical photometric and spectroscopic coverage of the superluminous supernova (SLSN) PS1-11ap, discovered with the Pan-STARRS1 Medium Deep Survey at z = 0.524. This intrinsically blue transient rose slowly to reach a peak magnitude of M_u = -21.4 mag and bolometric luminosity of 8 x 10^43 ergs^-1 before settling onto a relatively shallow gradient of decline. The observed decline is significantly slower than those of the superluminous type Ic SNe which have been the focus of much recent attention. Spectroscopic similarities with the lower redshift SN2007bi and a decline rate similar to 56Co decay timescale initially indicated that this transient could be a candidate for a pair instability supernova (PISN) explosion. Overall the transient appears quite similar to SN2007bi and the lower redshift object PTF12dam. The extensive data set, from 30 days before peak to 230 days after, allows a detailed and quantitative comparison with published models of PISN explosions. We find that the PS1-11ap data do not match these model explosion parameters well, supporting the recent claim that these SNe are not pair instability explosions. We show that PS1-11ap has many features in common with the faster declining superluminous Ic supernovae and the lightcurve evolution can also be quantitatively explained by the magnetar spin down model. At a redshift of z = 0.524 the observer frame optical coverage provides comprehensive restframe UV data and allows us to compare it with the superluminous SNe recently found at high redshifts between z = 2-4. While these high-z explosions are still plausible PISN candidates, they match the photometric evolution of PS1-11ap and hence could be counterparts to this lower redshift transient.

We present griz(P1) light curves of 146 spectroscopically confirmed Type Ia supernovae (SNe Ia; 0.03 < z < 0.65) discovered during the first 1.5 yr of the Pan-STARRS1 Medium Deep Survey. The Pan-STARRS1 natural photometric system is determined by a combination of on-site measurements of the instrument response function and observations of spectrophotometric standard stars. We find that the systematic uncertainties in the photometric system are currently 1.2% without accounting for the uncertainty in the Hubble Space Telescope Calspec definition of the AB system. A Hubble diagram is constructed with a subset of 113 out of 146 SNe Ia that pass our light curve quality cuts. The cosmological fit to 310 SNe Ia (113 PS1 SNe Ia + 222 light curves from 197 low-z SNe Ia), using only supernovae (SNe) and assuming a constant dark energy equation of state and flatness, yields w = -1.120(+0.360)(-0.206)(Stat)(+0.269)(-0.291)(Sys). When combined with BAO+CMB(Planck)+H-0, the analysis yields Omega(M) = 0.280(+0.013)(-0.012) and w = -1.166(+0.072)(-0.069) including all identified systematics. The value of w is inconsistent with the cosmological constant value of -1 at the 2.3 sigma level. Tension endures after removing either the baryon acoustic oscillation (BAO) or the H-0 constraint, though it is strongest when including the H-0 constraint. If we include WMAP9 cosmic microwave background (CMB) constraints instead of those from Planck, we find w = -1.124(+0.083)(-0.065), which diminishes the discord to <2 sigma. We cannot conclude whether the tension with flat ACDM is a feature of dark energy, new physics, or a combination of chance and systematic errors. The full Pan-STARRS1 SN sample with similar to three times as many SNe should provide more conclusive results.

We present a new satellite in the outer halo of the Galaxy, the first Milky Way satellite found in the stacked photometric catalog of the Panoramic Survey Telescope and Rapid Response System 1 (Pan-STARRS1) Survey. From follow-up photometry obtained with WFI on the MPG/ESO 2.2m telescope, we argue that the object, located at a heliocentric distance of 145+/-17 kpc, is the most distant Milky Way globular cluster yet known. With a total magnitude of M_V=-4.3+/-0.2 and a half-light radius of 20+/-2 pc, it shares the properties of extended globular clusters found in the outer halo of our Galaxy and the Andromeda galaxy. The discovery of this distant cluster shows that the full spatial extent of the Milky Way globular cluster system has not yet been fully explored.