adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Top: RV observations for TOI-6029 b, shown in red, with the full RV model shown in black. Bottom: residuals after removing the RV contribution from the transiting planet.
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Redshift vs. fibers for sky fibers (selected with OBJSTYPE=SKY criteria) for sky fibers from DESI Y1. In each panel, we also show the number of false positives selected using good redshift criteria (see Table 2) like true galaxy targets. The top panel shows results for BGS-like selection; the middle panel shows results for ELG-like selection, and the bottom panel presents the results for LRG-like redshift selection. The left panel (blue) shows the result for Redrock (without archetypes), and the right panels show the results of our archetype method (with a prior σ a = 0.1 on polynomial coefficients, shown in orange) in all panels. It is evident that the archetype performs 6%–40% better in rejecting false-positive redshifts for sky fibers.
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption: The rest-frame spectra of archetypes (shown as open circles in Figure 3) that can represent more sources than themselves in the parent galaxy sample. The number N shows how many galaxies in the parent sample the individual archetype can represent, i.e., with distances shorter than the minimum distances defined by the s 2 threshold in the SetCoverPy method. We can see a larger diversity in ELGs than in LRGs.
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption: The redshift comparison between the PCA-based Redrock method (left) and the archetype method (right), color-coded by their χ 2 difference for visually inspected galaxy spectra, reveals notable differences. The archetype method demonstrates reduced spurious clustering of redshifts and fewer catastrophic failures around z ∼ 1, 1.6. Furthermore, the archetype method generally yields lower χ 2 values, indicating better model fits.
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption:  g − r vs. r − z color–color space comparison between parent (left) and archetype (right) galaxies. The archetypes obtained with SetCoverPy span the properties of the parent sample well in this space. The colors are not corrected for interstellar extinction.
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Distribution of Legendre polynomial coefficients (in each camera, the constant term is in the top panel, and the slope term is in bottom panel) for sky fibers (for both dark and bright tiles) from the Y1 data set. The spread of distribution varies between 0.1 and 0.5 for dark tiles and between 0.2 and 1 for bright tiles. Based on this, we choose a prior value of 0.1 (lowest) on polynomial coefficients for our current archetype method. More details are presented in Section 3.2.
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: Representation of TOI-1437 b as it falls on a mass–radius diagram (large black circle). Individual solid lines are theoretical mass–radius curves for planets whose composition is specified in the figure legend. Light gray circles indicate the population of planets between 1.0 and 3.5 R ⊕ that have measured masses.
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: Left: transit model drawn from parameter posterior distributions fit from phase-folded TESS photometry of TOI-1437. The gray dots show the TESS 2 minutes cadence data. The orange line shows the best fit to each individual transit using exoplanet. The blue dots show the data binned to 2 minutes cadence. Right: phase-folded views of the best-fit RV model for TOI-1437 b (purple). Data from APF is shown in blue while HIRES is displayed in green, and each is binned to 12 total bins.
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 all features and PCA performance for the KN of GW170817. The labels/tags have the same meanings as in Figure 12. The mean coefficients of feature Nos. 15 and 16 are close to zero.
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 all features and PCA performance for DES15C2eaz. Again, the mean coefficients of feature Nos. 15 and 16 are close to zero, indicating that they are not effective (nearly half of the coefficients are negative).
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 all features and PCA performance for DC21bwbfe/SN2021bn (positive flux cases). The mean coefficients of feature Nos. 15 and 16 are small.
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: (Top) Phoenix forward model planetary spectrum corresponding to the dayside for WASP-121b. Emission lines from species such as CO are visible. (Bottom) The cross-correlation template Phoenix planetary spectrum generated by dividing by a median filter that removes the continuum emission.
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: NIRSpec G395H NRS2 spectrophotometry. Plotted is the WASP-121 spectra vs. detector integration number, which is proportional to time, with the color bar corresponding to the normalized flux. The transit can clearly be seen in the middle as well as the two eclipses at the top and bottom of the plot. The beginning and end of the transits and eclipses are marked with white horizontal lines.
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: The same as Figure 1 but plotting the residual spectrophotometry after removing the median stellar spectra, white-light phase curve, and phase-dependent planetary broadband emission spectrum.
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: Cross-correlation amplitude as a function of orbital phase and RV lag using the Phoenix model as a correlation template. The CCF amplitude has been normalized at each phase by its standard deviation. (Top) Correlation using a Phoenix grid model as a correlation template. (Bottom) Using a PHOENIX model template derived from a retrieval on the planetary dayside emission spectra. Vertical white lines mark transit and eclipse first and fourth contact phases.
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: The planetary RV signal derived using NIRSpec/NRS2 with 1σ uncertainties (black data points). A best-fit planetary RV signal is also shown (blue) as well as the eclipse and transit first and fourth contact phases (gray dashed lines). The RV data are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: Same as Figure 6 but for NIRSPec/NRS1. The RV data are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: Isochrone posterior values of the age vs. stellar density considering only the broadband magnitudes, parallax, and extinction (gray/black). An updated posterior with the added constraint of the JWST stellar density is also shown (red). The JWST-measured stellar density and isochrone age are indicated with the black data point, with 1, 2, and 3σ density confidence intervals shown (blue).
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: Illustration of the planet at orbital quadrature (phase 1.25) and the red/blueshifted velocity and day/night components. At this phase, the planet is redshifted from the orbital velocity, the dayside emission of the planet is blueshifted from winds and rotation, while the fainter nightside is redshifted from winds and rotation.
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: Same as Figure 4 but using a cross-correlation template derived from the data themselves.
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: Isochrones posterior distribution of stellar parameters (gray/black) along with the posterior constrained with the JWST transit-measured stellar density (red), with the values listed in Table 2.
Paper: An Absolute Mass, Precise Age, and Hints of Planetary Winds for WASP-121A and b from a JWST NIRSpec Phase Curve
Authors: David K. Sing, Thomas M. Evans-Soma, Zafar Rustamkulov, Joshua D. Lothringer, Nathan J. Mayne, Kevin C. Schlaufman
Figure caption: Dynamic RV stellar mass measurement compared to the stellar modeling mass constrained by the broadband photometry, distance, and stellar density.
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Moderate-resolution (R ≈ 2700) spectra of V1391 Cas on UT 2020 August 14.41. Spectra at each Echelle order are plotted in different colors. The absorption line profiles of Br-γ, Pa-β, Pa-γ, and Pa-δ in HD 5071 were removed during relative flux calibration (uncorrected profiles are shown by dashed lines). The influence of other H I lines was not removed from the reduced spectra. For comparison, the spectrum taken on UT 2020 August 17.54 (R. J. Rudy et al. 2024) is also plotted with a logarithmic scale bias.
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Moderate-resolution (R ≈ 2700) spectra of V1391 Cas. This figure provides a close-up view of the wavelength region from 11,700 to 14,050 Å (the dashed line is the same as in Figure 1).
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Moderate-resolution (R ≈ 2700) spectra of V1391 Cas. This figure provides a close-up view of the wavelength region from 9500 to 11,800 Å (the dashed line is the same as 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 fluxes in [O III] with the total fluxes of the continuum at 5100 Å (a) before correcting for the contribution of the stellar populations and (b) after correction. The corresponding parameters for the linear relations Log(L[O III]) ﹩=\,\alpha \times \mathrm{Log}(\lambda {\text{}}L[5100])+\beta ﹩ are given in Table 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: Alternative classification for RGs. In each panel, the solid curve separates SFGs from AGN. Left panel: RGs with intense emission lines (S/N ≥3), classified using the BPT diagrams (Figure 3). Middle panel: RGs with weak emission lines (S/N <3), but also classifiable using the BPT diagram. Right panel: RGs with nonmeasurable or undetected emission lines. The percentages refer to the number of galaxies relative to the total sample.
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 of redshifts (a) for our sample of galaxies with different AGN classes (omitting RGs classified as SFGs and TOs) and (b) only for the RGs with different AGN classes. The inset shows (on the same scale) a flat distribution for all the RGs without class distinction.
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: Reconstruction of the velocity profile of the line shown in Figure 14(a): v05, v10, v90, and v95 are the velocities in kilometers per second at the 5th, 10th, 90th, and 95th flux percentiles, respectively. These percentiles are determined by tracing the total flux cumulative function, where the line width is defined as W80 = v90 − v10 and the velocity offset as Δv = (v95 + v0.5)/2 (Harrison et al. 2014). In the absence of OF, Δv = 0 and W80 ∼ FWHM, where FWHM is the full width at half-maximum of the main Gaussian at 0 velocity.
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 EW([O III]) with λL[5100] as observed in (a) Sy2, (b) LINERs, (c) RG-Sy2, and (d) RG-LINERs. For each distribution we calculated two linear regressions, one on the whole sample (contour levels) and another on the medians of the cumulative percentiles (red bars), reducing the dispersion.
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: Alternative classification for (a) Sy2 and (b) LINERs using the WHAN 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: Comparing the WISE colors of PN and PAGBs with those of (a) Sy2 and LINERs and (b) all the RGs in our sample. Note that the few RGs consistent with PAGBs are in fact Sy2 in late-type spirals with high 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: Comparing the [O III] luminosities with the radio luminosities in (a) the RG-Sy2 and (b) the RG-LINERs. The black line is the division between high-excitation RGs (HERGs) and low-excitation RGs (LERGs) as proposed by Best & Heckman (2012): in general, HERGs have higher [O III] luminosities than LERGs. Note that while this separation criterion suggests most RG-Sy2 are HERGs, the classification of RG-LINERs as LERGs is less certain, since the bulk of their distribution (traced by the cumulative percentiles) falls almost right on the separation line.
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) Example of OF fitting using Gaussians. The green component is the main line, the blue is the OF, and the yellow is the sum of both (the red wing is not included). The red dashed lines are the rms consistent with S/N = 3. Note that the peak in OF is resolved, blueshifted by more than 69 km s−1. (b) Example of double OF: the second component in red is resolved and has S/N >3.