adsabs/AstroCLIMB huggingface dataset:
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: Ground-based transit observations of LHS 1678 c. The data points and curves are derived the same way as in Figure 12, but the binned data (white circles) are at 5 minutes cadence.
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: Posterior mass distributions for each planet resulting from our HARPS RV data modeling. We place 2σ and 3σ upper limits on the mass of each planet (corresponding to the usual 97.7% and 99.9% values, respectively), shown as color-coded arrows. The prior probability distribution is represented by a dashed gray line. The 3σ values correspond to bulk planet densities greater than iron, so we adopt the 2σ values as our upper limits.
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: TESS photometry folded on the planet periods. Purple dots are the individual 2 minute cadence measurements, and the vertical lines are 10 minute bins. The best-fit transit models described in the text are overlaid as green curves. Green shading corresponds to the central 68th percentile (1σ) range of models consistent with the data.
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: To demonstrate more clearly the ground-based detections of each planet, the ground-based light curves for planets b (left) and c (right; see Table 4) are stacked on top of each other and binned at 5 minutes cadence (white circles), with the transit model (black curve) overlaid.
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: Top: full HARPS RV time series with individual measurement uncertainties (black) along with the best-fit model and 1σ uncertainty (blue dashed line and shading). No significant RV signal is detected at the period of either planet nor is a significant RV trend. Bottom: RV residuals after removing the best-fit model.
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: Stability maps for π Men d. Yellow and green regions indicate binned values with a high probability of stability whereas dark regions are unstable. (Left) Stability regions in the eccentricity-planet-mass plane. (Middle) Stability regions in the of orbital-period planet-mass plane. (Right) Stability regions in the inclination-planet-mass plane.
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: Phase-folded RV variations and Keplerian orbit for π Men c. The contributions from planets b and d have been removed. Blue circles and red diamonds are nightly binned HARPS-POST and ESPRESSO RV measurements, respectively. The gray error bars include jitter. The curve represents the orbital solution. The zero phase of the RV curve corresponds to the time of first transit (see Table 6).
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: GLS periodogram of the activity indicators after removal of the dominant signal in each (Table 5). The vertical dashed line is the frequency of the 125 day period seen in the RV data.
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: RV variations and Keplerian orbit for π Men d phased to the orbital period of ∼125 days. The contributions from the inner and outer planets have been removed. Blue circles and red diamonds are nightly binned HARPS-POST and ESPRESSO RV measurements, respectively. The gray error bars include jitter. The curve represents the orbital solution. The zero phase of the RV curve corresponds to the time of inferior conjunction (see Table 6).
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: The time series of the S-index (top), FWHM (middle), and BIS (bottom) measurements extracted from the HARPS-Large data set. The red curves are sine fits using the period of the dominant peak in each periodogram (Table 5).
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: The RV vs. time from HARPS large program (blue circles) and ESPRESSO (red diamonds) nightly binned measurements for π Men d (125 day period) after removing the contribution of the inner and outer planets. The error bars include the jitter term. The curve represents the orbital solution.
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: The phase-binned BIS measurements using the ≈125 day period found in the RVs. The red curve represents an orbital solution to the 125 day period (see Section 5.1).
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: The FCO periodogram of the raw RV data. The red dashed vertical line marks the orbital period of the transiting planet.
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: S-index measurements over 16 consecutive nights. The curve represents the sine fit with a period of 18.7 days.
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: The error in the mass determination as a function of the number of measurements. The solid line represents a fit with error ∝  N −0.36. The red dashed lines represent a nominal error ∝  N −0.50 expected for white noise. The top red dashed line has its origin at the N = 70 data point.
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: The location of the radius valley from Van Eylen et al. (2018). The blue dashed line marks the hyperplane of maximum separation. The location of π Men c is marked by the red square.
Paper: A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
Authors: Artie P. Hatzes, Davide Gandolfi, Judith Korth, Florian Rodler, Silvia Sabotta, Massimiliano Esposito, Oscar Barragán, Vincent Van Eylen, John H. Livingston, Luisa Maria Serrano, Rafael Luque, Alexis M. S. Smith, Seth Redfield, Carina M. Persson, Martin Pätzold, Enric Palle, Grzegorz Nowak, Hannah L. M. Osborne, Norio Narita, Savita Mathur, Kristine W. F. Lam, Petr Kabáth, Marshall C. Johnson, Eike W. Guenther, Sascha Grziwa, Elisa Goffo, Malcolm Fridlund, Michael Endl, Hans J. Deeg, Szilard Csizmadia, William D. Cochran, Lucía González Cuesta, Priyanka Chaturvedi, Ilaria Carleo, Juan Cabrera, Paul G. Beck, Simon Albrecht
Figure caption: The location of π Men c in the mass–radius diagram for exoplanets with well-determined radii and masses (better to 15%). Composition models from Zeng et al. (2016) are displayed with different lines and colors.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: BPT (top) and WISE color–color (bottom) distributions for optical Type I AGN (T1; left), optical Type II AGN (T2; center left), BPT composite (Comp.; center right), and BPT star-forming (SF; right) for galaxies with a flux S/N > 3 in the represented emission lines. We note that T1 galaxies without a flux S/N > 3 in the BPT emission lines do not appear in the BPT diagram but are still counted in the totals. Typical WISE selection criteria are successful at excluding star-forming objects and preferentially select T1 objects, and AGNs are found throughout WISE color–color space. Refer to Figure 1 for a description of the BPT delineations, WISE color–color selection criteria, and error bars plotted in black.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: SED modeling for SDSS objIDs 1237678617934102742 (top figure) and 1237648674532295222 (bottom figure). In both instances, we show the SED fit with/without and AGN component with an extinction curve in the top/bottom panel. Both objects show strong evidence for requiring the AGN component in their modeling. In both objects, the W1−W2 color cannot be explained by the galaxy templates alone. While 1237678617934102742 shows evidence for an unobscured AGN, owing in part to an underprediction of the u-band flux by the galaxy templates, 1237648674532295222 is best fit by an obscured quasar, where there is little AGN emission visible in the optical.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: WISE color–color (top) and BPT (bottom) and distributions for Jarrett et al. (2011) selected (J11; left), Stern et al. (2012) selected (S12; center), and Mateos et al. (2012) selected (M12; right) objects. We note that T1 galaxies without a flux S/N > 3 in the represented lines do not appear in the BPT diagram but are still counted in the total. Typical WISE selection criteria are successful at excluding star-forming objects and preferentially select T1 objects. Refer to Figure 1 for a description of the BPT delineations, WISE color–color selection criteria, and error bars plotted in black.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: On the left, we plot the fraction of spectroscopic AGNs (both Type I and Type II) as a function of WISE mid-IR color space. We present our new color selection as a dotted–dotted–dashed line, designed to target spectroscopic AGNs. On the right, we plot the distribution of where our selected objects are found in BPT space for those objects with detected emission lines. Refer to Figure 1 for a description of the BPT delineations, WISE color–color selection criteria, and error bars plotted in black.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: Distributions of [O III]λ5007 Å luminosity for objects selected (black) and spectroscopic AGN not selected (orange) by different mid-IR color selection techniques. In the top panel, we show the count histogram, while in the bottom panel, we show the density histogram. The luminosity is corrected for galactic-scale extinction using the measured Balmer decrement. Typical mid-IR selection criteria are biased toward selecting a more luminous AGN population.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: Distributions of [O III]λ5007 Å luminosity for different mid-IR color selection techniques. In the top panel, we show the count histogram, while in the bottom panel, we show the density histogram. The luminosity is corrected for galactic-scale extinction using the measured Balmer decrement. The selection criteria presented in this work increases the completeness at all luminosities, but more notably at lower luminosities. This results in a median luminosity that is > 0.1 dex fainter than the other selection methods.