adsabs/AstroCLIMB huggingface dataset:
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: The results of photometric redshift estimation from the Bayesian analysis of the hydrodynamical simulation–based mock data for the CSST+Euclid-like survey employing the two SED models with the largest Bayesian evidence. By comparing with the results for the CSST-like survey in Figure 12, it becomes clear that the quality of photometric redshift estimation is obviously increased in both cases with and without noise. In particular, in the more realistic case with noise, the outliers caused by the misidentification of Lyman and Balmer break features are largely reduced. This suggests that the inclusion of the J, H, and Y bands from Euclid is helpful for improving the photometric redshift estimation. However, the more complicated β-τ form of SFH is not very helpful for improving the quality of photometric redshift estimation.
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: Same as Figure 8, but for the SFR. In general, the imperfect SED modeling is the more important source of error for the photometric SFR estimation of galaxies, though the contribution from observational noise is also very important. In particular, in the case without noise, it is clear that the simple τ model of SFH and the Calzetti et al. (2000) form of DAL lead to a severely biased estimation of SFR for the Horizon-AGN simulation–based mock sample of galaxies.
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: Same as Figure 12, but for the SFR. (a) By comparing with the results in Figure 10(c), it becomes clear that, with the additional consideration of metallicity evolution and the adoption of the DAL of Salim et al. (2018), the systematic bias and OLF of photometric SFR estimation are largely reduced, although the σ NMAD is slightly increased. (c) By additionally employing a more complicated β-τ form of SFH the quality of photometric SFR estimation increases to the best level. (b), (d) In the case with noise, the best two models are also very similar in their quality of photometric SFR estimation.
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: Same as Figure 12, but for the stellar mass. (a) By comparing with the results in Figure 9(c), it becomes clear that, with the additional consideration of metallicity evolution and the adoption of the DAL of Salim et al. (2018), the σ NMAD of photometric stellar mass estimation is reduced, although the bias and OLF are somewhat increased. (c) By additionally employing a more complicated β-τ form of SFH, the quality of photometric stellar mass estimation increases further. (b), (d) In the case with noise, the best two models are exactly the same in terms of the quality of photometric stellar mass estimation.
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: Same as Figure 8, but for the stellar mass. In general, the observational noise is the more important source of error for the photometric stellar mass estimation of galaxies, and the contribution from imperfect SED modeling is almost comparable.
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: An example of 1D and 2D posterior PDFs of free parameters obtained for the Bayesian analysis of a mock galaxy with CSST-like (gray), CSST+Euclid-like (red), and COSMOS-like (blue) photometric data. The contours show the 1σ, 2σ, and 3σ confidence regions, while the red dashed lines show the ground truth values of each parameter. It is clear that the parameters are more tightly constrained and some degeneracies between them are broken when using data sets with increasing discriminative powers.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: Top: F275W and F606W light curves (purple and orange, respectively) of 77 novae with observed brightness peaks in M87. Over-plotted are the 25th, 50th, and 75th percentiles (in order of brightness) of all of these F275W (in blue) and F606W (in red) light curves. Note that the computation of a percentile at a given time takes into account upper limit magnitude data points in individual nova light curves. To avoid clutter in this plot, those individual limit data points are not shown, but they can be seen in Table 3 and as arrows in Figure 15. The higher luminosities and slower rates of decline of novae in the NUV are apparent. Bottom: the F275W–F606W color curves of the M87 novae, as well as the 25th, 50th, and 75th percentiles of the color curves. Novae near maximum light exhibit m(F275W)–m(F606W) ∼ 0 ± 1, then become increasingly blue during the ensuing ∼30 days. After ∼30 days they remain at m(F275W)–m(F606W) ∼ −2 ± 0.5.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: The m(F275W)–m(F606W) color at the time of the observed visible peak vs. the visible peak magnitude (orange) and the color at the time of the observed NUV peak vs. the NUV peak magnitude (purple). The two data points for each of the 55 novae that are observed in both bands at the time of both peaks are connected by a thin line. The horizontal lines represent novae whose observed visible and NUV peaks occurred at the same epoch. The most luminous novae (those with peak magnitudes <23) achieve peak F275W and F606W brightnesses very close in time. Most (less luminous) novae exhibit fainter, redder F606W brightness peaks followed by more luminous, bluer F275W peaks.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: Top: the peak absolute magnitude distributions of 77 novae with observed peaks in 5 day cadence imagery of M87 in the F275W and F606W filters of HST, along with the median and standard deviations of the distribution. Novae are 0.9 mag more luminous at peak brightness in the NUV than in the visible. Bottom: a histogram of the peak F606W and F814W magnitudes from 1 day cadence imagery of M87 novae (Shara et al. 2016). Note that the median peak F606W magnitude from this 1 day cadence sample is almost identical to that of the 5 day cadence sample.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: Median HST light curve of 77 M87 novae with observed peaks in F275W bandpass (solid purple) and F606W bandpass (solid orange), both based on 5 day cadence observations. Also shown are the median daily cadence light curves of 32 M87 novae in the F814W bandpass (red) of HST from Shara et al. (2016). For each band, the 25th and 75th percentiles of all light curves in that band are shown as dotted lines. The much slower declines of novae in the NUV are apparent, as is the later rise to the peak of many novae in the NUV.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: F275W–F606W colors of 55 novae vs. the absolute peak F275W and F606W magnitudes. The arrows labeled “Time” indicate directions of color and magnitude change between the F606W and F275W peak brightnesses. As in Figure 10, we see that the most luminous novae (those with peak absolute magnitudes < −8) achieve peak F275W and F606W brightnesses very close in time.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: Top: F275W (violet) and F606W (yellow) peak magnitudes vs. t1 decline time for novae with observed peak brightnesses. Each nova is plotted in both filters, and the pairs of points for each nova are connected by a thin line. Faint, fast novae are as prevalent in the F275W bandpass as in the F606W bandpass. Bottom: Same as above except F275W and F606W magnitudes vs. t2 decline time.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: The normalized radial distributions of 94 M87 novae, and the K-band and F606W-band light of the galaxy. The novae are seen to closely track the galaxy K-band light. This is confirmed by the K-S test, which returns the statistic p = 0.61.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: The number of days after the observed F606W peak that the F275W peak was observed plotted vs. peak F606W magnitude (top), vs. peak F275W magnitude (middle), and as a histogram (bottom). Data from the 77 novae whose peaks were observed are included in the plots.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: Peak F275W vs. peak F606W absolute magnitudes of the 77 novae with observed peaks in M87. The correlations are given in the figure legend.
Paper: The Chandra Cygnus OB2 Legacy Survey: Design and X-Ray Point-source Catalog
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Tom L. Aldcroft, Vinay L. Kashyap, Francesco Damiani, Joe DePasquale, Antonella Fruscione
Figure caption: Left: the “as designed” Cygnus OB2 Chandra Legacy Survey tiling for the 36 30 ks pointings. The thick black box (bottom left) represents one ACIS-I pointing; the thin boxes represent all the pointings. Different colors show areas with different numbers of overlapping pointings: teal—four overlapping pointings; blue—two overlapping pointings; purple—one pointing. The black bars show roughly the relative dimensions of one pointing (∼16′), of the deep inner area (∼42′), and of the total field (∼56′). Pointing 1-1 lies at the lower right (SW), 1-6 lies at the upper right (NW), 6-1 lies at the lower left (SE), and 6-6 lies at the upper left (NE). Right: the “as executed” exposure map for the Cygnus OB2 Chandra Legacy Survey and complementary observations. The color bar gives the achieved effect exposure in units of ks. The deepest region of the survey with a nonnegligible area has an exposure time of ∼220 ks.
Paper: The Chandra Cygnus OB2 Legacy Survey: Design and X-Ray Point-source Catalog
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Tom L. Aldcroft, Vinay L. Kashyap, Francesco Damiani, Joe DePasquale, Antonella Fruscione
Figure caption: Distribution of various source quantities for the 7924 sources in the final X-ray catalog. Left: the distribution of net counts of all extracted sources, with quartiles at 7, 13, and 28 net counts. Middle: the background-subtracted median photon energy of all extracted sources, with quartiles at 1.7, 2.0, and 2.8 keV. Right: the distribution of model-independent source energy fluxes calculated using the equation ﹩{F}_{\mathrm{energy}}=1.602\times {10}^{-9}{\tilde{E}}_{\mathrm{photon}}\times {F}_{\mathrm{photon}}﹩ (see Section 5.2) with a median of 2.6 × 10−15 erg cm−2 s−1.
Paper: The Chandra Cygnus OB2 Legacy Survey: Design and X-Ray Point-source Catalog
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Tom L. Aldcroft, Vinay L. Kashyap, Francesco Damiani, Joe DePasquale, Antonella Fruscione
Figure caption: Example image of the Cyg X-3 readout streak in ObsID 10964 before (left) and after (right) application of a hard mask to remove events from the event file. Each image is approximately 5′ wide and aligned with north up and east to the left. The readout streak is oriented along a chip column, the position angle of which is dictated by the observation roll angle.
Paper: The Chandra Cygnus OB2 Legacy Survey: Design and X-Ray Point-source Catalog
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Tom L. Aldcroft, Vinay L. Kashyap, Francesco Damiani, Joe DePasquale, Antonella Fruscione
Figure caption: Final distribution of the 7924 X-ray sources in the Chandra Cygnus OB2 Legacy Survey after removing all sources that failed the source verification procedure (Section 4). The sources are color coded based on the detection method used to add the sources to the initial source candidate list. The 7608 surviving sources detected using either WAVDETECT or PWDetect (mostly detected using both codes) are colored gray. The 216 surviving sources detected using the Enhanced WAVDETECT code (but not detected by other methods) are colored red, and the 100 surviving sources added from known source lists (and not detected by other methods) are colored blue.
Paper: The Chandra Cygnus OB2 Legacy Survey: Design and X-Ray Point-source Catalog
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Tom L. Aldcroft, Vinay L. Kashyap, Francesco Damiani, Joe DePasquale, Antonella Fruscione
Figure caption: An inverted three-color (RGB = soft 0.5–1.2 keV/medium 1.2–2.0 keV/hard 2–7 keV) X-ray image of the center of Cyg OB2 showing observations from the Cygnus OB2 Chandra Legacy Survey. The X-ray data have been processed, cleansed, and flux-calibrated as described in the text. The image is approximately ﹩23^{\prime} \times 17^{\prime} ﹩, with north up and east to the left. The brightest X-ray sources visible in this image are predominantly OB stars, with the six most luminous objects in the center of the image being the Trapezium of Cyg OB2 #8 (upper left), #9 and #22 (middle and lower left), the blue hypergiant Cyg OB2 #12 and MT267 (middle right), and Cyg OB2 #5 (upper right). See Negueruela et al. (2008) for a near-IR image with a similar field of view. Many hundreds of lower-mass stellar X-ray sources are also visible.
Paper: The Chandra Cygnus OB2 Legacy Survey: Design and X-Ray Point-source Catalog
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Tom L. Aldcroft, Vinay L. Kashyap, Francesco Damiani, Joe DePasquale, Antonella Fruscione
Figure caption: Top: histogram of the exposure times in all observations used in this work. The narrow peaks lie at the 1, 2, and 4 exposure values generated from the overlapping gridded observations. Peaks are also visible at ∼80 and ∼140 ks, where, respectively, three and five grid pointings overlap owing to variations in the roll angles of neighboring ObsIDs, as well as at ∼170 and ∼220 ks, where the existing 50 and 100 ks observations overlap with the central area of four grid pointings. The broader bases correspond to overlaps caused by slight variations in the roll angles of the ObsIDs.
Paper: The Chandra Cygnus OB2 Legacy Survey: Design and X-Ray Point-source Catalog
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Tom L. Aldcroft, Vinay L. Kashyap, Francesco Damiani, Joe DePasquale, Antonella Fruscione
Figure caption: Distribution of various observational and technical quantities for the 7924 sources in the final X-ray catalog. Left: the number of times each source is observed. The majority of sources (>80%) are observed at least four times owing to the tiling strategy outlined in Section 2.1. Middle: the smallest off-axis angle at which any source is observed, with quartiles at 2.′3, 3.′2, and 4.′0. Right: the positional uncertainty of all sources, with quartiles at 0.″2, 0.″3, and 0.″5.
Paper: The Chandra Cygnus OB2 Legacy Survey: Design and X-Ray Point-source Catalog
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Tom L. Aldcroft, Vinay L. Kashyap, Francesco Damiani, Joe DePasquale, Antonella Fruscione
Figure caption: Distribution of X-ray sources in the Chandra Cygnus OB2 Legacy Survey colored as a function of the lowest off-axis angle that the source is detected at. The observational tiling strategy is evident in the grid pattern seen in this image. Due to the tiling strategy used, the vast majority of sources were observed at least once at an off-axis angle <4′ and therefore with PSF sizes <2″ in radius (at 1.49 keV).
Paper: The GW Vir Instability Strip in Light of New Observations of PG 1159 Stars: Discovery of Pulsations in the Central Star of A72 and Variability of RX J0122.9–7521
Authors: Paulina Sowicka, Gerald Handler, David Jones, John A. R. Caldwell, Francois van Wyk, Ernst Paunzen, Karolina Bąkowska, Luis Peralta de Arriba, Lucía Suárez-Andrés, Klaus Werner, Marie Karjalainen, Daniel L. Holdsworth
Figure caption: Top: Gaia magnitude distribution of the observed sample of 29 PG 1159 stars. Bottom: distribution of the median noise level achieved in the survey.
Paper: The GW Vir Instability Strip in Light of New Observations of PG 1159 Stars: Discovery of Pulsations in the Central Star of A72 and Variability of RX J0122.9–7521
Authors: Paulina Sowicka, Gerald Handler, David Jones, John A. R. Caldwell, Francois van Wyk, Ernst Paunzen, Karolina Bąkowska, Luis Peralta de Arriba, Lucía Suárez-Andrés, Klaus Werner, Marie Karjalainen, Daniel L. Holdsworth
Figure caption: Light curves and their respective Fourier amplitude spectra of the survey targets. Plots for different stars are separated with horizontal lines. Light curves: note different scales. Fourier spectra: they were calculated up to their respective Nyquist frequencies but are plotted until 1200 day−1.  Dashed lines show the detection threshold of S/N ≥4. Note different scales.
Paper: The GW Vir Instability Strip in Light of New Observations of PG 1159 Stars: Discovery of Pulsations in the Central Star of A72 and Variability of RX J0122.9–7521
Authors: Paulina Sowicka, Gerald Handler, David Jones, John A. R. Caldwell, Francois van Wyk, Ernst Paunzen, Karolina Bąkowska, Luis Peralta de Arriba, Lucía Suárez-Andrés, Klaus Werner, Marie Karjalainen, Daniel L. Holdsworth
Figure caption: Light curves and Fourier amplitude spectra of two SAAO observing runs on the central star of planetary nebula A72. The Fourier amplitude spectra were calculated up to the Nyquist frequency but are shown up to 1200 day−1. Insets show a zoomed-in view into the frequency range of detected pulsations. Dashed lines show the detection threshold of S/N ≥ 4. Note the same scales for the light curves and Fourier spectra.
Paper: The GW Vir Instability Strip in Light of New Observations of PG 1159 Stars: Discovery of Pulsations in the Central Star of A72 and Variability of RX J0122.9–7521
Authors: Paulina Sowicka, Gerald Handler, David Jones, John A. R. Caldwell, Francois van Wyk, Ernst Paunzen, Karolina Bąkowska, Luis Peralta de Arriba, Lucía Suárez-Andrés, Klaus Werner, Marie Karjalainen, Daniel L. Holdsworth
Figure caption: Light curves and Fourier amplitude spectra of two SAAO observing runs on RX J0122.9–7521. The Fourier amplitude spectra were calculated up to the Nyquist frequency but are shown up to 1200 day−1. Insets show a zoomed-in view into the frequency range of the detected variations. Dashed lines show the detection threshold of S/N ≥ 4. Note the same scales for the light curves and Fourier spectra.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: Left: histograms of the t1 decline times in F275W and F606W of 77 novae in M87. The much slower t1 declines in the NUV are apparent. Right: histograms of the t2 decline times in F275W and F606W of 77 novae in M87. The declines in the NUV are slightly slower than in the visible, but much less so than for the t1 decline times.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: Peak apparent magnitude, t1 decline time, and (F275W–F606W) color at peak brightness of the novae in M87 that had observed peaks. The lack of correlations means that novae of all luminosities, speed classes are origins are thoroughly mixed in the galaxy.