adsabs/AstroCLIMB huggingface dataset:
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: Density distribution in redshift of galaxies with different AGN spectral classes and where OFs are detected.
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: BPT diagnostic diagram for the RGs with emission lines compared with photoionization models calculated by Bennert et al. (2006a).
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: BPT diagnostic diagram comparing Sy2 and LINERs in our sample with two samples of PN: high-excitation (black crosses) and low-excitation (black diamonds).
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 line ratios [S II]λλ6717, 6731/Hα with [N II]λ6584/Hα in all the RGs with emission lines (both subsamples with different S/N are used): (a) SFGs, (b) TOs, (c) Sy2, and (d) LINERs. Note that there is almost no difference between Sy2 and TOs in this diagram.
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: Classification of AGN using standard (BPT) diagnostic diagram: (a) for Sy2 and (b) for LINERs. The different zones are as defined in Kauffmann et al. (2003), Kewley et al. (2006), and Torres-Papaqui et al. (2012a).
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: BPT diagrams for RGs with emission lines, (a) with S/N ≥3 and (b) with S/N <3. The AGN type separations are the same as those in Figure 1.
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 line ratios [S II]λλ6717, 6731/Hα with [N II]λ6584/Hα (Torres-Papaqui et al. 2012b), and identifying the zones with typical values for SFGs and AGN, in (a) Sy2 and (b) LINERs. Note the huge overlap between the distributions.
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: Results of max-t tests comparing (a) the stellar mass of the host (M stellar) and (b) the 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: Results of max-t tests comparing AGN with OF with those without OF: (a) stellar mass of host and (b) stellar ages.
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: Results of max-t tests comparing AGN with OF with those without OF: (a) redshift, (b) morphology, 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: Variation of sBHAR vs. sSFR in AGN with different classes (black, RG; green, LINER; blue, Sy2; and red, Sy1) at different redshifts (circle, redshift range (0, 0.1]; square, (0.1, 0.2]; lozenge, (0.2, 0.3]; and triangle, (0.3, 0.4]; a filled symbol identifies an AGN with OF).
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: Results of max-t tests comparing AGN with OF with those without OF: (a) BH mass, (b) BHAR, and (c) Eddington ratios.
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: Results of max-t tests comparing (a) BH masses (M BH) and (b) Eddington ratios (N Edd).
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: Results of max-t tests comparing (a) AGN luminosities, L AGN = λ L(5100), and (b) BHARs.
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: Increases in mass of BHs and host stellar populations with the redshift. The colors and symbols have the same meanings as in Figure 26: circle, (0, 0.1]; square, (0.1, 0.2]; lozenge, (0.2, 0.3]; and triangle, (0.3, 0.4].
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 for the intensity of the wind W80 (a) in different AGN classes and (b) in radio-detected (R) and not radio-detected galaxies.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Visual galaxy detection model (Faster-RCNN). The backbone is used to extract features of the input image and generate feature maps of the input image. The RPN module utilizes feature maps producing some boxes that may contain targets. Then a box feature extractor future extracts features and feeds them into the box classifier and box regressor to obtain final results. The model first trains on the galaxy-star data set to help the model acquire the capability of detecting and distinguishing between galaxies and stars. Then finetune it on the galaxy pair data set.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Four types of galaxy pairs in the training data set. In each row, the images belong to the same category, arranged from top to bottom as “close,” “projection-separated,” “edge-on,” and “irregular” targets sequentially.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Procedures of the galaxy pair detection and sample reduction.
Paper: The TESS-Keck Survey. XXII. A Sub-Neptune Orbiting TOI-1437
Authors: Daria Pidhorodetska, Emily A. Gilbert, Stephen R. Kane, Thomas Barclay, Alex S. Polanski, Michelle L. Hill, Keivan G. Stassun, Steven Giacalone, David R. Ciardi, Andrew W. Boyle, Steve B. Howell, Jorge Lillo-Box, Mason G. MacDougall, Tara Fetherolf, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Isabel Angelo, Corey Beard, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Joseph M. Akana Murphy, Malena Rice, Ryan Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Edward W. Schwieterman
Figure caption: Spectral energy distribution of TOI-1437. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit PHOENIX atmosphere model (black). The inset shows the absolute flux-calibrated Gaia spectrum as a gray swathe overlaid on the model.
Paper: The TESS-Keck Survey. XXII. A Sub-Neptune Orbiting TOI-1437
Authors: Daria Pidhorodetska, Emily A. Gilbert, Stephen R. Kane, Thomas Barclay, Alex S. Polanski, Michelle L. Hill, Keivan G. Stassun, Steven Giacalone, David R. Ciardi, Andrew W. Boyle, Steve B. Howell, Jorge Lillo-Box, Mason G. MacDougall, Tara Fetherolf, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Isabel Angelo, Corey Beard, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Joseph M. Akana Murphy, Malena Rice, Ryan Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Edward W. Schwieterman
Figure caption: Results of the blended source confidence (BSC) analysis of Calar Alto Lucky imaging data indicate that the probability for TOI-1437 to have a blended, undetected, eclipsing binary capable of mimicking our transit is very low (0.076%).
Paper: The TESS-Keck Survey. XXII. A Sub-Neptune Orbiting TOI-1437
Authors: Daria Pidhorodetska, Emily A. Gilbert, Stephen R. Kane, Thomas Barclay, Alex S. Polanski, Michelle L. Hill, Keivan G. Stassun, Steven Giacalone, David R. Ciardi, Andrew W. Boyle, Steve B. Howell, Jorge Lillo-Box, Mason G. MacDougall, Tara Fetherolf, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Isabel Angelo, Corey Beard, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Joseph M. Akana Murphy, Malena Rice, Ryan Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Edward W. Schwieterman
Figure caption: Companion sensitivity for speckle imaging. Contrast curves (5σ) for 562 nm are shown in blue and 832 nm in red. The reconstructed 832 nm speckle image (top right) shows that no close companions to TOI-1437 were detected within the obtained contrast and angular limits.
Paper: The TESS-Keck Survey. XXII. A Sub-Neptune Orbiting TOI-1437
Authors: Daria Pidhorodetska, Emily A. Gilbert, Stephen R. Kane, Thomas Barclay, Alex S. Polanski, Michelle L. Hill, Keivan G. Stassun, Steven Giacalone, David R. Ciardi, Andrew W. Boyle, Steve B. Howell, Jorge Lillo-Box, Mason G. MacDougall, Tara Fetherolf, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Isabel Angelo, Corey Beard, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Joseph M. Akana Murphy, Malena Rice, Ryan Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Edward W. Schwieterman
Figure caption: Companion sensitivity for the near-infrared adaptive optics imaging. The black points represent the 5σ limits and are separated in steps of 1 FWHM; the purple represents the azimuthal dispersion (1σ) of the contrast determinations. The inset image is of the primary target showing no additional close-in companions.
Paper: The TESS-Keck Survey. XXII. A Sub-Neptune Orbiting TOI-1437
Authors: Daria Pidhorodetska, Emily A. Gilbert, Stephen R. Kane, Thomas Barclay, Alex S. Polanski, Michelle L. Hill, Keivan G. Stassun, Steven Giacalone, David R. Ciardi, Andrew W. Boyle, Steve B. Howell, Jorge Lillo-Box, Mason G. MacDougall, Tara Fetherolf, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Isabel Angelo, Corey Beard, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Rae Holcomb, Jack Lubin, Andrew W. Mayo, Joseph M. Akana Murphy, Malena Rice, Ryan Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Edward W. Schwieterman
Figure caption: Target pixel file corresponding to TOI-1437 observations by TESS in Sector 14. Sources from Gaia DR3 are shown as red circles, with their size corresponding to the magnitude contrast against TOI-1437 (marked with the label “1” and a white cross). The aperture used by the TESS-SPOC pipeline is shown as a shaded red region in each panel.
Paper: Unveiling Subarcsecond Multiplicity in the Pleiades with Gaia Multicolor Photometry
Authors: Dmitry Chulkov
Figure caption: Deviation of radial velocity δ ν = ∣ν − ν  c ∣ (color coded) from the reference ν  c  = 5.69 km s−1, depending on the relative proper motion δ μ (Equation (1)), and parallax deviation, defined as ﹩{\rm{\Delta }}\varpi /{\sigma }_{\varpi }=(\varpi -{\varpi }^{c})/\sqrt{{\sigma }^{2}+{\sigma }_{c}^{2}}﹩. ϖ  c  and σ  c  are the cluster’s average parallax and dispersion according to Y. Tarricq et al. (2022; Table 1), ϖ ± σ is the reported Gaia DR3 parallax for a given star. Sources with δ μ and Δϖ/σ  ϖ  values close to zero are superimposed in the plot. The absolute majority of them fall into the δ ν < 5 km s−1 range, but a few stars with deviating radial velocities are still present. For most of them, it can be explained by the disturbance from the neighboring source within 1″–2″; however, two stars marked by ◯ show δ ν ≳ 15 km s−1 according to both Gaia and APOGEE data, suggesting they may be field stars. Their faint magnitudes (G ∼ 14.7 and 14.8mag) imply large uncertainties, while their position in the color–magnitude diagram (Figure 4) is consistent with being a cluster member, so their membership is not completely ruled out. In the plot, bare points · are used for probable cluster members. Sources considered to be field stars are marked with □, while stars surrounded by ◯ have controversial status. Notably, all probable members meet the ∣Δϖ/σ  ϖ ∣ < 5.5 condition, regardless of the δ μ value. Several objects outside this range are given controversial status if their radial velocity and position in the color–magnitude diagram do not contradict cluster membership.
Paper: Unveiling Subarcsecond Multiplicity in the Pleiades with Gaia Multicolor Photometry
Authors: Dmitry Chulkov
Figure caption: Parallaxes and RUWE for the G < 15mag sample, restricted by relative proper motion. Left: δ μ < 5 mas yr−1 (Equation (1)). 377 stars with available parallax in Gaia DR3 are shown. Two entries with reliable low-RUWE solutions, ϖ = 12.55 ± 0.03 and ϖ = 2.65 ± 0.02 mas, are marked by □ and considered to be foreground and background objects, respectively. Their Gaia DR3 radial velocities, ν = −6.1 ± 0.2 and 27.2 ± 1.9 km s−1, along with positions in the color–magnitude diagram (Figure 4), confirm these sources are unrelated to the Pleiades. Among entries with RUWE < 2.5, the star marked by ◯ shows the largest parallax, ϖ = 8.19 ± 0.02 mas, which places it less than 14 pc from the cluster’s center. Since its radial velocity perfectly matches that of the cluster, it is considered to be a probable member. The smallest ϖ for the star with low RUWE is 6.40 ± 0.02 mas, corresponding to a distance of 20 pc from the center. Its Gaia DR3 radial velocity ν = −0.5 ± 0.3 also suggests that this star (marked by ◯) is unrelated to the Pleiades. Finally, the brightest (G < 4.5mag) cluster members are marked by ×, all of which show RUWE excess. Two stars with G < 4.5mag are not shown: Alcyone, which has a two-parameter solution, and Asterope, with δ μ ∼ 7.5 mas yr−1 according to Gaia DR3. Right: previously discussed sources with δ μ < 5 mas yr−1 are shown with black dots, objects with 5 < δ μ < 10 mas yr−1 are colored red. While the newly introduced subsample contains many background sources, several stars such as Asterope (marked ◯, G = 4.2mag) are certain Pleiades members.
Paper: Unveiling Subarcsecond Multiplicity in the Pleiades with Gaia Multicolor Photometry
Authors: Dmitry Chulkov
Figure caption: The relative proper motion distribution (δ μ, Equation (1)) for all sources with G < 15mag within a two degree radius centered on the reference coordinates from Y. Tarricq et al. (2022). δ μ = 10 mas yr−1 corresponds to a tangential speed of 6.4 km s−1 at the Pleiades distance. Left: 6047 stars with a full astrometric Gaia DR3 solution. Right: 82 objects with a two-parameter solution in Gaia DR3, for which the proper motion from PPMXL is used. Note the larger fraction of sources meeting the δ μ < 5 mas yr−1 threshold, indicating likely cluster membership, for these entries.
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: OGLE variables in the Galactic Bulge in the r band: eclipsing variable OGLE-BLG-ECL-277767 (top; P = 0.406 day; 5 s exposures) and RR Lyrae variable OGLE-BLG-RRLYR-12257 (middle; P = 0.318 day; 50 s exposures) with the original light curves (top, middle) and the phase-folded version (bottom; we use the period value from OGLE to shift the data points). For the RR Lyrae variable, after the direct image flux (totFlux) cut mentioned earlier and a cut on significant outliers, in the bottom row we also remove outliers in the difference image flux (psFlux) by using a 3σ cut around the median, and remove data points that have significantly large error bars (1/10 of the light-curve amplitude) to produce light curves cleaner than in the top row. In the difference images, the annular rings around bright stars are mainly caused by saturation, but they do not affect our targets. The observing condition metrics are estimated from the header information of instcal, as these are not included in qcInv. The guider transparency is not available for the top panel exposures, and we give the airmass ﹩\sec (z)﹩ instead; the sky brightness shows a similar trend to the airmass.
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: Evolution of the feature quantiles (q  i , where i is the feature index) and the feature coefficients (c  i , on the first principal component) of the target (KN of GW170817; matched by coordinate within 1″). The X-axis corresponds to individual exposures in chronological order (four exposures here), and we omit the exact exposure number (or observation time) for clarity. The circular marker color shows the PSF flux S/N (a redder color corresponds to a higher S/N) on the difference image. The gray squares give the coefficients of a feature on the first principal component for different exposures; the hollow squares give the (sign flipped) negative values; the horizontal dotted line shows one divided by the square root of the number of features. We also present the time evolution of the first component EVR, the quantile of the first component value of the target compared to other sources (q P), and the teff (τ). Additionally, we give the mean coefficient value 〈c  i 〉, with the fraction of positive values (f +), and the mean quantile value 〈q  i 〉 among exposures. The gray curve in the q P diagram gives the mean of all feature quantiles of the target, in order to test the effectiveness of PCA candidate selection.
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: Example of running PCA on the DECam data set for GW170817 KN. Top: we give the observation time, visit/exposure number, and CCD number. Then, we show the effective exposure time, and “EVR” means explained variance ratios of the first and second principal components. The title also lists the PSF flux S/N on the difference image. Left: the first (PC1) and second (PC2) principal component values of sources in the transformed space. Those points are all remaining sources after flag filtering (Section 4.1). The target (KN) is marked by an orange point. Middle: the coefficient of each feature along each principal component direction (i.e., the projection on the principal component vector). Hollow markers indicate the negative values (sign flipped). The reference horizontal dotted line denotes one divided by the square root of the number of features (﹩\sqrt{1/15}\sim 0.26﹩), showing the effectiveness of each feature. Right: the feature quantiles of the target (i.e., the fraction of sources that have a value for this feature smaller than or equal to that of the target). The horizontal dashed line gives the PC1 quantile of the target among sources, showing the effectiveness of candidate selection (R/B).
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: Examples of running PCA on the DES15C2eaz data (Type II SN). We use the same color scheme as Figure 11. Note that even though the teff is low for the top exposure, PCA still separates the target well from other sources (q P = 1).
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: DECam DDF SN (Type Ia) DC21bwbfe/SN2021bnv in the g, r, and i bands. Note that the host galaxy affects the light curves of the object on the direct images (totFlux), but the light curves from the difference images (psFlux) are much cleaner.
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: DECam DDF SN candidate DC21cove in the g, r, and i bands. For clarity, we use individual diagrams for each band, instead of displaying all light curves on the same set of axes.