adsabs/AstroCLIMB huggingface dataset:
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Left and middle panels: light curves of the KN of GW170817 in the g band from the forced photometry of the difference image and direct image, respectively. We give the celestial coordinates (R.A., decl.) in the title. Here, psFlux is the point-source PSF flux from the difference image, while totFlux is from the direct (science) image. The gray vertical tick in each light-curve diagram shows the time of the difference/direct image on the right. The “midPointTai” means the International Atomic Time (Temps Atomique International in French, TAI) at the middle of the exposure. Underneath, we provide the weather metrics—seeing (FWHM θ in arcseconds) and the effective exposure time teff obtained from qcInv for reference. For the exposures, we consider that seeing has the greatest impact on teff compared to other observing conditions such as transparency, sky brightness, and airmass. The horizontal dashed lines give the thresholds of poor weather conditions (teff = 0.15 and θ = 1.″6), and the triangle markers highlight the conditions worse than the thresholds. Right panels: the difference image from the first day (i.e., the flux peak; visit 668963 at CCD 36, MJD 57983.977; 300 × 300 pix; North on the top and East on the left; scaled by arcsinh), together with the processed science (direct) image and the template. The target (KN) is at the image center. The source near the right edge of the difference image is probably from a variable star.
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Flow chart of the MMA pipeline steps described in this paper. The arrows show the data flow. The blue rectangles describe the input data. The green rectangles show the pipeline steps from the LSST Science Pipelines software. The yellow rectangles give the steps for Real/Bogus classification (R/B) to generate per-exposure candidates and weights. The orange rectangles show the output (the places that our data product can be fed into). The dashed arrows and the steps enclosed by the dashed rectangle are optional (Section 4.6).
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: DES SN (Type II): 15C2eaz in the r band observed with 150 s exposures (top) and 16X3jj in the i band observed with 10 s exposures (bottom).
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: HiTS SN (both in the g band). Top panels: Blind15A_07_N2_1215_3860 (SNHiTS15H). Bottom panels: Blind15A_12_S28_0091_2772 (SNHiTS15bd). The blank regions are caused by CCD edges. Even though there is a bias artifact in the template, the pipeline still produces clean light curves. These two objects are both from the HiTS labeled set for ML training and thus have high credibility. We titled them with their names in HiTS (year, field, CCD, and pixel coordinates). The presentation and format here (and in the following Figures) are the same as in Figure 2.
Paper: Characterization of Blue and Yellow Straggler Stars of Berkeley 39
Authors: Komal Chand, Khushboo K. Rao, Kaushar Vaidya, Anju Panthi
Figure caption: (a) The spatial distribution, (b) proper motion distribution, and (c) parallax distribution using ML-MOC algorithm on Gaia DR3 data. The member information data is available as the data behind the figure associated with Figure 2.
Paper: Characterization of Blue and Yellow Straggler Stars of Berkeley 39
Authors: Komal Chand, Khushboo K. Rao, Kaushar Vaidya, Anju Panthi
Figure caption: (a) H-R diagram showing the single-component BSSs as blue open triangles and YSSs as pink open squares. BSSs with excess in more than one filter are shown as stars, whereas BSSs with excess in one filter are shown as open circles. The cooler component of BSS16 (most probably a BL or just a binary star) is shown with a green open star, and the hot companion associated with it is shown in a green solid star. An orange dotted curve represents a 6 Gyr PARSEC isochrone, and the ZAMS is depicted as a black dashed curve. Various solid gray curves represent low mass (LM) and ELM WD cooling curves of different masses, sourced from J. A. Panei et al. (2007) and L. G. Althaus et al. (2013). (b) The hot companion of BSS16 (most probably a BL or just a binary star) lies near the ELM WD cooling curves of 0.186 M ⊙ (J. A. Panei et al. 2007), indicating its approximate cooling age.
Paper: Characterization of Blue and Yellow Straggler Stars of Berkeley 39
Authors: Komal Chand, Khushboo K. Rao, Kaushar Vaidya, Anju Panthi
Figure caption: (a) Spatial distribution of the cluster members as gray data points, BSS marked with blue open circles and YSS marked with green open squares. (b) Optical CMD of cluster members of Berkeley 39 identified using the ML-MOC algorithm on Gaia DR3 members. The cluster members, along with their probabilities, are shown with auxiliary colors. The BSSs and YSSs are represented by blue open circles and green open squares, respectively. A PARSEC isochrone (A. Bressan et al. 2012) of age = 6 Gyr, distance = 4200 pc, extinction, A  G  = 0.41 mag, and color-excess E(BP − RP) = 0.16 mag is overplotted on the CMD. The ZAHB is shown as a green dashed line and black dashed line shows equal-mass binary isochrone. The machine-readable table for this figure is available in the online version of the article.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Characterization of Blue and Yellow Straggler Stars of Berkeley 39
Authors: Komal Chand, Khushboo K. Rao, Kaushar Vaidya, Anju Panthi
Figure caption: The binary-component SED of BSS16. The top panel displays the double-component SED of each object, with blue data points representing extinction-corrected flux values (labeled as “Observed flux”) and black error bars showing flux errors. The green dashed line represents the cool component fit (labeled as “A”), while the brown dashed line represents the hot (B) component fit (labeled as “B”), with orange curves representing iteration residuals. The composite fit is depicted as a pink curve (labeled as “Model”), with gray data points denoting data points that were not included in the fits (labeled as “No fit”). The fractional residual for single (green) and composite (pink) fits is shown in the bottom panel. On the x-axis, black error bars represent fractional errors (labeled as “Fractional error”). The cool and hot component parameters derived from the SED, as well as the estimated errors, are listed at the top of the plots.
Paper: Characterization of Blue and Yellow Straggler Stars of Berkeley 39
Authors: Komal Chand, Khushboo K. Rao, Kaushar Vaidya, Anju Panthi
Figure caption: The single-component SED fits of BSS and YSS candidates. The top panels in each figure show extinction-corrected observed fluxes in brown data points, with black error bars representing the errors in observed fluxes, and the blue curve representing the Kurucz stellar model fit. The bottom panels depict the residual between extinction-corrected observed fluxes and the model fluxes across the filters from UV to IR wavelengths. The gray data points are not included in the fitting. The dashed line in the lower panel represents a fractional residual of 0.3.
Paper: Characterization of Blue and Yellow Straggler Stars of Berkeley 39
Authors: Komal Chand, Khushboo K. Rao, Kaushar Vaidya, Anju Panthi
Figure caption: The single-component SED fit of BSS having fractional residual greater than 0.3 in at least two UVOT filters. The symbols and curves mean the same as in Figure 3.
Paper: Characterization of Blue and Yellow Straggler Stars of Berkeley 39
Authors: Komal Chand, Khushboo K. Rao, Kaushar Vaidya, Anju Panthi
Figure caption: The single-component SED fits of BSS having fractional residual less than 0.3 in all but in one UVOT filter. The symbols and curves mean the same as in Figure 3.
Paper: Discovery of RR Lyrae in the Ultra-faint-dwarf Galaxy Virgo III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: Products of χ 2 and MAD as a function of mean r-band magnitudes. The left panel is for simulated light curves, including constant stars (gray points), ab-type RR Lyrae (circles), and c-type RR Lyrae (squares). The color bar represents the input amplitudes for the simulated light curves. The inset figure is the zoomed-in version to highlight constant stars. The red line, given as χ 2 × MAD = 0.045 r − 0.875, is adopted to separate RR Lyrae and constant stars. The right panel is for those stars, classified in SDSS DR16, with LOT light curves. The red line is same as the line shown in the inset figure on the left panel. We identified three RR Lyrae labeled as V1, V2, and V3. The light curve for the star with χ 2 × MAD ∼ 4.5 was affected by outliers, and hence it was rejected as a RR Lyrae candidate.
Paper: Discovery of RR Lyrae in the Ultra-faint-dwarf Galaxy Virgo III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: A deep-stack image, created by the median, combined all of the LOT images using SWARP (Bertin et al. 2002). The cyan ellipses, centered at ﹩(\alpha ,\delta {)}_{J2000}^{\mathrm{Virgo}\ \mathrm{III}}﹩, have semimajor axes of {1, 2, 3, 4} × r  h , a projected ellipticity ϵ = 1 − a/r  h  (where a is the projected semiminor axis, and r  h  is the half-light radius in arcminute), and with a position angle of θ. Values for ﹩(\alpha ,\delta {)}_{J2000}^{\mathrm{Virgo}\ \mathrm{III}}﹩, r  h , ϵ, and θ are all adopted from Homma et al. (2023). Locations of the three detected RR Lyrae were also shown in this deep-stack image.
Paper: Discovery of RR Lyrae in the Ultra-faint-dwarf Galaxy Virgo III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: Folded r-band light curves for the two ab-type RR Lyrae V1 and V2. The dashed curves are the best-fit template light curves returned from the gatspy’s periodic.RRLyraeTemplateModeler module. The template light curves were adopted from Sesar et al. (2010).
Paper: A Close Binary Lens Revealed by the Microlensing Event Gaia20bof
Authors: E. Bachelet, P. Rota, V. Bozza, P. Zieliński, Y. Tsapras, M. Hundertmark, J. Wambsganss, Ł. Wyrzykowski, P. J. Mikołajczyk, R. A. Street, R. Figuera Jaimes, A. Cassan, M. Dominik, D. A. H. Buckley, S. Awiphan, N. Nakhaharutai, S. Zola, K. A. Rybicki, M. Gromadzki, K. Howil, N. Ihanec, M. Jabłońska, K. Kruszyńska, K. Kruszyńska, U. Pylypenko, M. Ratajczak, M. Sitek, M. Rabus
Figure caption: (Left) The source trajectories (blue), caustics (red) and critical curves (black) for the eight models. Note that the center of mass of the lenses is kept fixed at (0,0). The microlensing astrometric deflections in R.A. (middle) and in decl. (right) vs. time are also displayed. The color indicates the observed Gaia G magnitude.
Paper: Discovery of RR Lyrae in the Ultra-faint-dwarf Galaxy Virgo III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: Comparison of r-band amplitudes (upper panel) and absolute magnitudes (lower panel) of the three detected RR Lyrae in Virgo III to the RR Lyrae in the globular clusters (orange and cyan symbols; adopted from Ngeow et al. 2022).
Paper: Discovery of RR Lyrae in the Ultra-faint-dwarf Galaxy Virgo III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: Comparison of the input (true) periods and the periods found, using the gatspy package, for our simulated RR Lyrae light curves. The black dashed lines are for the cases of P found = (±5%)P true. The various colors dotted curves represent the aliasing periods.
Paper: Discovery of RR Lyrae in the Ultra-faint-dwarf Galaxy Virgo III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: Same as Figure 4, but for the c-type RR Lyrae V3.
Paper: The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies
Authors: Juan Pablo Torres-Papaqui, Roger Coziol, Aitor C. Robleto-Orús, Karla A. Cutiva-Alvarez, Paulina Roco-Avilez
Figure caption: (a) Violin plots comparing the morphologies of AGN with OFs (identified as A) and without OF (identified as B). The equivalent in terms of Hubble types is (0, E), (1, S0), (2, Sa), (3, Sb), (4, Sc), (5, Sd), and (6, Im), with intermediate mixed types, for example, (0.5, E/S0), (1.5, S0/Sa), etc. (b) Comparison of SFRs.
Paper: The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies
Authors: Juan Pablo Torres-Papaqui, Roger Coziol, Aitor C. Robleto-Orús, Karla A. Cutiva-Alvarez, Paulina Roco-Avilez
Figure caption: (a) Violin plots comparing the morphology of the host in the different AGN types. The equivalent in terms of Hubble types is (0, E), (1, S0), (2, Sa), (3, Sb), (4, Sc), (5, Sd), and (6, Im), with mixed types, for example, (0.5, E/S0), (1.5, S0/Sa), etc. Comparison of (b) SFRs, (c) stellar masses M *, and (d) ages of the oldest stellar populations, t old.
Paper: The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies
Authors: Juan Pablo Torres-Papaqui, Roger Coziol, Aitor C. Robleto-Orús, Karla A. Cutiva-Alvarez, Paulina Roco-Avilez
Figure caption: (a) Violin plots comparing the intensity of the OFs in the different AGN types. (b) Same comparison distinguishing between AGN not detected in radio and those detected (adding R to their class).
Paper: The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies
Authors: Juan Pablo Torres-Papaqui, Roger Coziol, Aitor C. Robleto-Orús, Karla A. Cutiva-Alvarez, Paulina Roco-Avilez
Figure caption: Comparing the means and quartiles of the sBHAR and sSFR of RG-AGN with (a) LINERs, (b) Sy2, and (c) Sy1. All values are in logarithm exponents. Different symbols distinguish radio-quiet from radio-loud; filled/open symbols are galaxies with OF/without OF. The three markers of galaxy evolution, horizontal, diagonal, and vertical lines, are explained in the text.
Paper: The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies
Authors: Juan Pablo Torres-Papaqui, Roger Coziol, Aitor C. Robleto-Orús, Karla A. Cutiva-Alvarez, Paulina Roco-Avilez
Figure caption: Max-t test comparing the host characteristics of galaxies with different AGN types: (a) redshift (z), (b) morphology (T), and (c) SFR.
Paper: The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies
Authors: Juan Pablo Torres-Papaqui, Roger Coziol, Aitor C. Robleto-Orús, Karla A. Cutiva-Alvarez, Paulina Roco-Avilez
Figure caption: Comparing the SFR with the intensity of the wind, W80, in (a) Sy1, (b) RGs, (c) Sy2, and (d) LINERs.
Paper: The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies
Authors: Juan Pablo Torres-Papaqui, Roger Coziol, Aitor C. Robleto-Orús, Karla A. Cutiva-Alvarez, Paulina Roco-Avilez
Figure caption: Violin plots comparing for the different AGN types the (a) AGN luminosity, (b) BHAR, (c) BH mass, and (d) Eddington ratio.
Paper: The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies
Authors: Juan Pablo Torres-Papaqui, Roger Coziol, Aitor C. Robleto-Orús, Karla A. Cutiva-Alvarez, Paulina Roco-Avilez
Figure caption: Comparing the stellar masses with the SMBH masses in (a) LINERs vs. Sy2 and (b) LINERs vs. RGs. The solid line is the relation established by Reines & Volonteri (2015).
Paper: The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies
Authors: Juan Pablo Torres-Papaqui, Roger Coziol, Aitor C. Robleto-Orús, Karla A. Cutiva-Alvarez, Paulina Roco-Avilez
Figure caption: Violin plots comparing AGN with OF (A) and without OF (B): (a) stellar mass of host, (b) BHAR, (c) BH mass, and (d) Eddington ratios.
Paper: LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
Authors: Dennis Zaritsky, Giulia Golini, Richard Donnerstein, Ignacio Trujillo, Mohammad Akhlaghi, Nushkia Chamba, Mauro D'Onofrio, Sepideh Eskandarlou, S. Zahra Hosseini-ShahiSavandi, Raúl Infante-Sainz, Garreth Martin, Mireia Montes, Javier Román, Nafise Sedighi, Zahra Sharbaf
Figure caption: Recovered completeness as a function of g-band central surface brightness and angular size on average across the survey. For guidance, we plot the locations of two well-known UDGs, DF 44 and NGC 5846-UDG1, if they are placed at the median LIGHTS distance (15.2 Mpc). The photometric data for DF 44 comes from D. Zaritsky et al. (2023), while that for NGC 5846-UDG1 comes from D. A. Forbes et al. (2019). We also show the upper end of the r  e  range of the galaxies we have found with the dashed line. We are highly complete in such systems to a central surface brightness approaching ∼27 mag arcsec−2. We note, however, that the lowest surface brightness Milky Way satellite known, Antlia 2 (G. Torrealba et al. 2019), lies at μ 0,g  = 30 mag arcsec−2, assuming V − g = −0.3 and μ 0 = μ  e  −1 (A. P. Ji et al. 2021), and is well beyond our capability to detect with this survey.
Paper: LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
Authors: Dennis Zaritsky, Giulia Golini, Richard Donnerstein, Ignacio Trujillo, Mohammad Akhlaghi, Nushkia Chamba, Mauro D'Onofrio, Sepideh Eskandarlou, S. Zahra Hosseini-ShahiSavandi, Raúl Infante-Sainz, Garreth Martin, Mireia Montes, Javier Román, Nafise Sedighi, Zahra Sharbaf
Figure caption: Low surface brightness candidate satellite galaxies identified around LIGHTS galaxies (Table 4). Each panel is ∼1.′5 on a side, with north at the top. The color images are created by combining the g and r bands using astscript-color-faint-gray (R. Infante-Sainz & M. Akhlaghi 2024).
Paper: LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
Authors: Dennis Zaritsky, Giulia Golini, Richard Donnerstein, Ignacio Trujillo, Mohammad Akhlaghi, Nushkia Chamba, Mauro D'Onofrio, Sepideh Eskandarlou, S. Zahra Hosseini-ShahiSavandi, Raúl Infante-Sainz, Garreth Martin, Mireia Montes, Javier Román, Nafise Sedighi, Zahra Sharbaf
Figure caption: The eight candidates that we reject as background galaxies on the basis of visual appearance, although a few (SMDG0240159-081842, SMDG1220572+085721, and SMDG1223543+160013) might indeed be satellites. The images are ∼70″ on a side and north is up.
Paper: LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
Authors: Dennis Zaritsky, Giulia Golini, Richard Donnerstein, Ignacio Trujillo, Mohammad Akhlaghi, Nushkia Chamba, Mauro D'Onofrio, Sepideh Eskandarlou, S. Zahra Hosseini-ShahiSavandi, Raúl Infante-Sainz, Garreth Martin, Mireia Montes, Javier Román, Nafise Sedighi, Zahra Sharbaf
Figure caption: The LIGHTS sample to date in the morphology-absolute magnitude space. The star represents the Milky Way for comparison, with an adopted absolute magnitude of M  r  = −21.64 (J. Bland-Hawthorn & O. Gerhard 2016) and a morphological classification of Sbc (P. W. Hodge 1983; R. C. J. Kennicutt 2001).
Paper: Flaring Activity for Low-mass Stars in the β Pictoris Moving Group
Authors: Jordan N. Ealy, Joshua E. Schlieder, Thaddeus D. Komacek, Emily A. Gilbert
Figure caption: The rate of flares above 1031.5 erg compared to the stellar rotation period. The rates derived in this sample are shown in color as a function of spectral type. The gray points plotted underneath are the results from Medina et al. (2020). The flaring rates found for this sample are systematically consistent with the field M-dwarf flaring rates. The βMPG sample also occupies the “saturated” regime, where with decreasing rotation period the flaring rate remains fairly constant. Due to the fine sampling of flare injection, the recovery probability of the flares in this sample is well determined.
Paper: Flaring Activity for Low-mass Stars in the β Pictoris Moving Group
Authors: Jordan N. Ealy, Joshua E. Schlieder, Thaddeus D. Komacek, Emily A. Gilbert
Figure caption: The flare-finding results for stella (red) and AltaiPony (N 3 = 2, 3;  blue, yellow) mark where each program defines the peak of a flare within a light curve excerpt for TIC 268637115. Without any adjustments to the standard number of points above the baseline, the number and characteristics of the flares found overlap about half the time. Tuning the AltaiPony parameters leads to better agreement. The flare near 1398.5 MBJD is only recovered by AltaiPony with N 3 = 2 and stella. Since AltaiPony relies on an outlier cut it reliably finds large flares, while stella focuses on finding a characteristic shape. A closer look at the flagged stella times shows more nonclassical flares. By tuning to maximize their agreement on visually confirmed flares, we determine the optimal AltaiPony parameters for this data set.
Paper: Flaring Activity for Low-mass Stars in the β Pictoris Moving Group
Authors: Jordan N. Ealy, Joshua E. Schlieder, Thaddeus D. Komacek, Emily A. Gilbert
Figure caption: The maximum (blue), median (yellow), and minimum (magenta) energy flares detected for each star are listed with their spectral type in equivalent duration (ED, top) and TESS band energy (bottom) space. In energy space, the median energy of flares remains flat with later spectral type. This also implies an intrinsic connection between the mechanism generating flares and the mass of the star. This is accompanied by a decreased effective temperature, so while the total energy decreases, the comparative UV flux delivery compared to the blackbody of the star increases. Another notable feature is the flat maximum EDs and accompanying downward shift in energy space as an anticipated change with decreasing luminosities.
Paper: Flaring Activity for Low-mass Stars in the β Pictoris Moving Group
Authors: Jordan N. Ealy, Joshua E. Schlieder, Thaddeus D. Komacek, Emily A. Gilbert
Figure caption: Flare frequency distributions for β Pictoris low-mass stellar sample split between early-type (orange) and mid/late-type (purple) stars. The denser sampling close to the lower-energy regime is indicative of the overall prevalence of low-energy flares compared to those of high energy. The average power law for this sample is α = 1.58 ± 0.23 with a similar overlap for both populations. The inset shows a nonnegligible difference between FFDs though the distribution has a relatively normal shape. This is due to the intrinsic variability of activity in our sample, driven by differences in spin-down timescales and internal dynamos across the low-mass regime. All FFDs occupy a similar parameter space, with early types showing a broader spread to smaller flares for similar rates. In addition to these natural variations, some FFDs are not fit well by a single power law due to their morphology. Of note, the largest flares in this sample are mostly from later-type stars.