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: (a)–(c) Archival and TESS imaging of LHS 1678 and the surrounding sky demonstrating its motion across the sky from 1983 to late-2018 when TESS observations were acquired. Each image spans a ﹩1\buildrel{\,\prime}\over{.} 5\times 1\buildrel{\,\prime}\over{.} 5﹩ field of view approximately centered on the LHS 1678 Gaia DR2 coordinates, represented as a plus symbol. Made via Lightkurve (Lightkurve Collaboration et al. 2018) and labeled to match (a) and (b), (c) includes several bright Gaia DR2 sources as faint red dots to anchor the location of the closest bright sources in the earlier images. LHS 1678 dominates the flux detected by TESS, with no bright sources at its current location. There are, however, two faint sources nearby. (d) The TESS Sector 5 TPF image of LHS 1678 produced using the tpfplotter software package (Aller et al. 2020). The image spans 11 × 11 pixels with a pixel scale of 21″ pixel−1. The TESS SPOC pipeline photometric extraction aperture used to produce the Sector 5 light curve is shown as red shaded squares. Numbered red dots reveal the locations of Gaia DR2 sources with sizes scaled to their ΔG relative to LHS 1678. The faint sources #2 and #3 lie within the TESS aperture. We rule out these sources as the transit hosts via dilution arguments and follow-up observations (see Section 4.1).
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: Nearly 10 yr of ASAS-SN data show no clear signs of stellar rotation. Left: astropy-generated LS periodograms of the LHS 1678 photometry. Horizontal lines denote false alarm probabilities (FAPs). Vertical lines denote the planet orbital periods, the 41.7 day HARPS signal to be discussed in Section 4.3, and the highest peak in the g-band LS periodogram at 192.5 days. Note that the peak in the g-band LS periodogram at one day is likely caused by observations being performed only at night in Chile and/or South Africa, and peaks at less than one day are likely associated aliases. We do not see any peaks in the V-band LS periodogram. Right: g-band ASAS-SN photometry folded on the candidate 192.5 day period found using the LS periodogram. Black circles are the data binned at a 15 minutes cadence, with error bars corresponding to the standard deviation of the magnitude values in each bin. We do not see clear signs of periodicity.
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: A cross-correlation analysis focusing on strong TiO absorption bands in the CHIRON spectra of LHS 1678 reveals no evidence for double lines (top) and a single-peaked cross-correlation function (bottom). These analyses rule out very close-in, unresolved binary companions. The stability of LHS 1678's RV measured by CHIRON over the full observing baseline further excludes the possibility of a spectroscopic companion orbiting across a range of masses and periods (Table 6). The vertical, dashed lines labeled s and t in the cross-correlation plot indicate where the sky and telluric lines would be; our template does not correlate with those lines.
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: Normalized red-optical spectrum of LHS 1678 observed using RC Spec at the CTIO/SMARTS 1.5 m in 2005. The spectrum exhibits deep absorption bands from TiO, VO, and CaH from ∼6000–8000 Å, a characteristic of M dwarfs. We do not see the strong CaHn (n = 1–3) and TiO5 bands typically associated with cool subdwarfs (Gizis 1997). Following the methodology described in Henry et al. (2002), the spectrum yields a type M2.0V.
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: CTIO/SMARTS 0.9 m observations spanning ∼16 yr reveal that LHS 1678 exhibits notably low magnetic activity. As a function of time, we examine the difference in V  J  magnitude relative to the mean magnitude of all observations (middle line). The standard deviation is 7.6 mmag; the top and bottom lines mark twice the standard deviation.
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: VLT NaCo adaptive-optics image of LHS 1678 (inset) and corresponding 5σ contrast sensitivity curve with a 1σ error bar. Flux in the inset image is in log scale, ranging from 0 to 100 detector units, with the core of the stellar point-spread function (PSF) saturated. No companions are detected down to the contrast limits, including the astrometrically detected companion described in Section 3.
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: Simulated semimajor axes of a photocentric orbit for LHS 1678 based on RECONS astrometry data. Four different scenarios are simulated based on the assumptions of the semimajor axes of 17 and 100 mas, and the periods of 42 and 100 yr. The white dashed line indicates equal-mass components, and the region above this line is not physical. Blue lines mark 0.08 M ⊙, and yellow lines mark the change of grid sizes from 0.01 to 0.002 M ⊙. Red boxes highlight the possible systems which can produce the observed perturbations. There is no red box in the 100 mas/42 yrs case because there are no mass combinations consistent with the astrometric 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: Phase-folded light curves of TOI-696.03 identified in a search of the full two-cycle, four-sector TESS data set using two independent analyses. Top (Analysis 1): the gray and purple symbols are averages of TESS 2 minute observations in intervals of 3.6 and 12 minutes in phase, respectively. The best-fit model is plotted in red. Bottom (Analysis 2): gray and green symbols represent 2 minute cadence and 7.5 minute binned measurements, respectively. The brown symbols are drawn from the best-fit transit model from this analysis. Both analyses consistently yield a small planet candidate on a 4.965 day period. If confirmed, TOI-696.03 would be sub-Earth-sized and near the 4:3 mean-motion resonance with LHS 1678 c.
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: SED of LHS 1678 with best-fit stellar model used to determine an alternate set of stellar parameters. 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 NextGen atmosphere model (black).
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: Top: the GLS periodogram of the HARPS-Large RV measurements after removing the motion of the outer planet (orbital frequency, f 1 = 4.79 × 10−4 day−1). Middle: the GLS periodogram of the RV residuals after removing the contribution of the dominant peak at f 2 = 0.008 day−1. Bottom: the GLS periodogram of the final RV residuals after removing the orbital frequency of the transiting planet, f 3 = 0.16 day−1.
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: Left: the difference between out-of-transit and in-transit images of LHS 1678 star during transits of TOI-696.03 reveal that the star is the location of the candidate transits and rule out other nearby stars as the transit host (small dots). Right: a zoom in on LHS 1678 in the difference image.
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 GLS periodograms of the activity indicators extracted from the HARPS-Large data set. From top to bottom: S-index, FWHM, and BIS. The vertical dashed line marks the orbital frequency of the 125 days detected in the RVs.
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: Top: the RV time series from UCLES (brown squares), HARPS-PRE (red circles), and HARPS-POST (blue triangles). For clarity we do not plot the ESPRESSO measurements, as these are contemporaneous with the HARPS-POST data. The curve is the Keplerian orbital solution for π Men b. Bottom: the residuals after subtracting the orbit of π Men b.
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: Growth of the LS power of the 125 day period attributed to a third body in the system as a function of the number of RV measurements for the real data (HARPS-Large and ESPRESSO; blue circles) and simulations (red triangles).
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: SDSS f  r /f  g  vs. f  g /f  u  distributions of the SDSS Legacy MGS (left), our WISE Matched S/N sample (center), and our WISE S/N Rejected sample (right). In the top panels, we plot the low-redshift regime (0 < z ≤ 0.15) of the samples and in the bottom panels, we show the high-redshift regime (z > 0.15). We show the Strateva et al. (2001) u − r = 2.22 separator as a dashed line above which galaxies are typically thought to be early-type, with late-type galaxies living below the separator. In the bottom right of each panel, we show the fraction of objects that lie above the Strateva et al. (2001) separator, while in the bottom left of each panel, we show the fraction that lie below the separator. Most objects (>85%) that do not satisfy our WISE S/N criteria are characterized by red colors and are found along the “red-sequence,” especially at higher redshifts. These objects are likely early-type galaxies with lower star formation rates and diminished infrared emission, so called “red-and-dead” galaxies.
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: The WISE color–color and BPT diagnostic distributions of the WISE Matched S/N sample presented in this work. In the left panel, we plot the BPT diagnostic for objects in our WISE Matched S/N sample with a flux S/N > 3 detection in each of the BPT emission lines. The Kauffmann et al. (2003a; dashed) and Kewley et al. (2001; solid) diagnostic curves are plotted as well. In the right panel, we plot the WISE color–color distribution of our WISE Matched S/N sample. Selected AGN color selection criteria are overplotted: the Jarrett et al. (2011) box (solid), the Mateos et al. (2012) wedge (dashed), and the Stern et al. (2012) line (dotted–dashed). In both panels, we present orange contours encompassing 68%, 95%, and 99.7% of the corresponding plotted sample and show error bars corresponding to the median uncertainty in the bottom-right corner.
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 emission line fluxes compared between GELATO and the MPA-JHU catalog, ALPAKA, and the S11 study. For each line, we restrict to objects that have at least one component detected at the 3σ level with GELATO. For the MPA-JHU catalog, we only compare the narrow components, while for the remaining studies, we compute the total GELATO flux in each line as a sum of all detected components. For each line, the GELATO fluxes are are compared to the total flux from all line components for each study. In each panel, we show error bars corresponding to three times the median GELATO uncertainty in the bottom-right corner.