adsabs/AstroCLIMB huggingface dataset:
Paper: Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy
Authors: Dongwook Lim, Andreas J. Koch-Hansen, Seungsoo Hong, Sang-Hyun Chun, Young-Wook Lee
Figure caption: Difference in [X/H] between SVO 3206a and SVO 3206b stars, with ±1σ error, as a function of condensation temperature of elements. The dashed line indicates a least-squares fit, and the dotted line denotes the value of 0.0 dex in Δ[X/H]. The p-value of the Pearson correlation test is written in the upper right corner.
Paper: Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy
Authors: Dongwook Lim, Andreas J. Koch-Hansen, Seungsoo Hong, Sang-Hyun Chun, Young-Wook Lee
Figure caption: Toomre diagram for our wide binary samples. The curved dashed and dotted lines represent total velocities of 180 and 70 km s−1, which divide the halo, thick disk, and thin disk. Our samples dynamically belong to the thin disk.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: GCLFs are shown as absolute V-band magnitude histograms for each galaxy. The accepted universal turnover is marked with a solid vertical line at M  V  = −7.4 mag, while a dashed vertical line is used to mark the magnitude limit of M  V  = −6.8 that we adopt to divide between “faint” and “bright” cluster popluations. The top left panel shows the luminosity function of GCs in the Milky Way (Harris 1996, 2010). We fit a Gaussian to the luminosity function of GCs in the Milky Way, where the V-band magnitudes are taken from the most recent version of the Milky Way GC catalogs. The best fit, shown in red in the top left panel, has a peak near M  V  ≈ −7.30 ± 0.12 mag and a dispersion parameter σ = 1.20 ± 0.08 mag, very similar to the parameters found earlier by Secker (1992) for the Milky Way GCLF.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: Radial density distributions of bright (blue) and faint (red) GCs (divided at M  V  = −6.8) are plotted using equal-size radial bins. The profiles for NGC 628 are on the left and for NGC 3627 on the right. Error bars are calculated as Poissonian statistics. The best-fit de Vaucouluer (dashed) and exponential (dotted) profiles to each distribution are shown.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: The best-fit age and reddening (E(B-V)) from the default PHANGS-HST pipeline for all color-selected GC candidates from the human-classified catalogs in the top panel and the ML-classified candidates in the bottom. Objects classified by us as likely GCs after visual inspection are shown in blue and contaminants are shown in red. We expect GCs to have estimated ages ≥ 1 Gyr (dashed line), but only ≈25% do. This illustrates the challenges of breaking the age–reddening–metallicity degeneracy using a single set of SSP model parameters, as discussed extensively in Whitmore et al. (2023) and D. A. Thilker et al. (2024, in preparation).
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: Color BVI images showing examples of contaminants from our initial color selection of GC candidates. The left image shows a background galaxy that was included in the ML catalogs. The center panel shows two background galaxies also from the ML-selected catalogs, while the right panel shows a saturated foreground star from the human-classified catalog. All contaminants are removed from the final GC catalogs.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: The locations of all likely GCs are overplotted on a V-band image of their host galaxy, NGC 628 (left) and NGC 3627 (right). The bright GCs (M  V  < −6.8) are indicated by blue circles and faint ones (M  V  > −6.8) are in red. The ellipses show the approximate distance where the radial density of the faint GC population peaks: 2.5 kpc for NGC 628 and 4.5 kpc for NGC 3627.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: Total number of color-selected GC candidates from the human-classified catalogs (left bar) and the “bright” (same magnitude range) ML-classified catalogs (right bar). Each bar is broken into likely GCs (blue) and contaminants (red).
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: This figure shows BVI 2″ × 2″ postage stamp images for 16 representative GCs from the human catalog. The clusters are all spherical and centrally concentrated, but show a range of colors. Most are isolated with the exception of cluster 3529 in NGC 3351, which is found in the bulge.
Paper: PHANGS Hubble Space Telescope Treasury Survey: Globular Cluster Systems in 17 Nearby Spiral Galaxies
Authors: Matthew Floyd, Rupali Chandar, Bradley C. Whitmore, David A. Thilker, Janice C. Lee, Rachel E. Pauline, Zion L. Thomas, William J. Berschback, Kiana F. Henny, Daniel A. Dale, Ralf S. Klessen, Eva Schinnerer, Kathryn Grasha, Médéric Boquien, Kirsten L. Larson, Sinan Deger, Ashley T. Barnes, Adam K. Leroy, Erik Rosolowsky, Thomas G. Williams, Leonardo Úbeda
Figure caption: The total number of color-selected candidate GCs are shown for each galaxy in the sample. The contaminants are shown in red and likely GCs in blue. NGC 3627 is an outlier due to the large number of faint candidates selected by the ML algorithm.
Paper: TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star
Authors: Emma Page, Joshua Pepper, Duncan Wright, Joseph E. Rodriguez, Robert A. Wittenmyer, Stephen R. Kane, Brett Addison, Timothy Bedding, Brendan P. Bowler, Thomas Barclay, Karen A. Collins, Phil Evans, Jonathan Horner, Eric L. N. Jensen, Marshall C. Johnson, John Kielkopf, Ismael Mireles, Peter Plavchan, Samuel N. Quinn, S. Seager, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Joshua N. Winn, George Zhou, Carl Ziegler
Figure caption: Mass–radius diagram for 39 transiting brown dwarf companions. TOI-1994b is marked with a red “x.” The colored lines represent isochrones for brown dwarfs at ages 0.1, 0.5, 1, 5, and 10 Gyr (Baraffe et al. 2003). Points are colored by the age of the system from publications. Gray represents systems published with a large age range.
Paper: TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star
Authors: Emma Page, Joshua Pepper, Duncan Wright, Joseph E. Rodriguez, Robert A. Wittenmyer, Stephen R. Kane, Brett Addison, Timothy Bedding, Brendan P. Bowler, Thomas Barclay, Karen A. Collins, Phil Evans, Jonathan Horner, Eric L. N. Jensen, Marshall C. Johnson, John Kielkopf, Ismael Mireles, Peter Plavchan, Samuel N. Quinn, S. Seager, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Joshua N. Winn, George Zhou, Carl Ziegler
Figure caption: Eccentricity vs. brown dwarf mass for 39 transiting brown dwarf companions. The color represents the orbital period of the system. Squares represent hosts with temperatures below the Kraft break (T eff ≈ 6250) and stars represent hosts with temperatures above the Kraft break. A vertical line shows the population split at 42.5 M  J  proposed by Ma & Ge (2014). TOI-1994b is marked with a red “x.”
Paper: TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star
Authors: Emma Page, Joshua Pepper, Duncan Wright, Joseph E. Rodriguez, Robert A. Wittenmyer, Stephen R. Kane, Brett Addison, Timothy Bedding, Brendan P. Bowler, Thomas Barclay, Karen A. Collins, Phil Evans, Jonathan Horner, Eric L. N. Jensen, Marshall C. Johnson, John Kielkopf, Ismael Mireles, Peter Plavchan, Samuel N. Quinn, S. Seager, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Joshua N. Winn, George Zhou, Carl Ziegler
Figure caption: Discovery light curves from TESS for TOI-1994b using 2 minutes cadence data from the SPOC pipeline from Sector 36 (blue dots) and 30 minutes cadence data from the QLP pipeline from Sectors 9 and 10 (green diamonds). The black line represents a model fit from the EXOFASTv2 described in Section 3. The curves are phase folded to a period of 4.0337142 days. The residuals for the best fit model are shown in the bottom panel.
Paper: TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star
Authors: Emma Page, Joshua Pepper, Duncan Wright, Joseph E. Rodriguez, Robert A. Wittenmyer, Stephen R. Kane, Brett Addison, Timothy Bedding, Brendan P. Bowler, Thomas Barclay, Karen A. Collins, Phil Evans, Jonathan Horner, Eric L. N. Jensen, Marshall C. Johnson, John Kielkopf, Ismael Mireles, Peter Plavchan, Samuel N. Quinn, S. Seager, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Joshua N. Winn, George Zhou, Carl Ziegler
Figure caption: Radial velocities for TOI-1994 from CHIRON and three MINERVA-Australis telescopes. The black line represents the global fit model from the EXOFASTv2 described in Section 3. The curve is phase folded to a period of 4.0337142 days. The residuals for the best-fit model are shown below the radial velocity curve.
Paper: TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star
Authors: Emma Page, Joshua Pepper, Duncan Wright, Joseph E. Rodriguez, Robert A. Wittenmyer, Stephen R. Kane, Brett Addison, Timothy Bedding, Brendan P. Bowler, Thomas Barclay, Karen A. Collins, Phil Evans, Jonathan Horner, Eric L. N. Jensen, Marshall C. Johnson, John Kielkopf, Ismael Mireles, Peter Plavchan, Samuel N. Quinn, S. Seager, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Joshua N. Winn, George Zhou, Carl Ziegler
Figure caption: HR diagram for 39 transiting brown dwarf companions. TOI-1994b is marked with a red “x.” The solid blue lines represent the instability strip as given by Dupret et al. (2005). Points are colored by the mass of the brown dwarf companions.
Paper: TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star
Authors: Emma Page, Joshua Pepper, Duncan Wright, Joseph E. Rodriguez, Robert A. Wittenmyer, Stephen R. Kane, Brett Addison, Timothy Bedding, Brendan P. Bowler, Thomas Barclay, Karen A. Collins, Phil Evans, Jonathan Horner, Eric L. N. Jensen, Marshall C. Johnson, John Kielkopf, Ismael Mireles, Peter Plavchan, Samuel N. Quinn, S. Seager, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Joshua N. Winn, George Zhou, Carl Ziegler
Figure caption: Ground-based light curves taken in B, Rc and PANSTARRS z-short passbands plotted with corresponding models. The depth of the transit is consistent across these passbands.
Paper: TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star
Authors: Emma Page, Joshua Pepper, Duncan Wright, Joseph E. Rodriguez, Robert A. Wittenmyer, Stephen R. Kane, Brett Addison, Timothy Bedding, Brendan P. Bowler, Thomas Barclay, Karen A. Collins, Phil Evans, Jonathan Horner, Eric L. N. Jensen, Marshall C. Johnson, John Kielkopf, Ismael Mireles, Peter Plavchan, Samuel N. Quinn, S. Seager, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Joshua N. Winn, George Zhou, Carl Ziegler
Figure caption: Speckle imaging from SOAR of TOI-1994. The points represent 5σ detection sensitivity and the inset displays ACF from SOAR. No stellar companions are found within 3″ down to the detection limits.
Paper: TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star
Authors: Emma Page, Joshua Pepper, Duncan Wright, Joseph E. Rodriguez, Robert A. Wittenmyer, Stephen R. Kane, Brett Addison, Timothy Bedding, Brendan P. Bowler, Thomas Barclay, Karen A. Collins, Phil Evans, Jonathan Horner, Eric L. N. Jensen, Marshall C. Johnson, John Kielkopf, Ismael Mireles, Peter Plavchan, Samuel N. Quinn, S. Seager, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Joshua N. Winn, George Zhou, Carl Ziegler
Figure caption: Discovery light curves from TESS for TOI-1994b using 2 minute cadence data from the SPOC pipeline from Sector 36 (blue dots) and 30 minute cadence data from the QLP pipeline from Sectors 9 and 10 (green diamonds).
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: The PDFs of emission of the galactic disk (r ≥ 1 kpc) after masking the center, at 7.7, 10, 11.3, and 21  μm for NGC 4321. Top: images of the galactic disk of NGC 4321 in each MIRI filter, with the masked central region shaded. Middle: PDFs of inclination-corrected intensity from each image excluding the masked central region. The colors in the PDF reflect the color bar in intensity used to display each image. Vertical dashed lines indicate rms noise levels in each filter. Bottom: the same disk-only PDFs shown in the middle row, but now with the y-axis in log-stretch to highlight features at the high-intensity end. The PDFs of the disk show a consistent lognormal component that peaks at lower intensities, as well as a high-intensity tail that can be roughly approximated to a power law.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: Images and PDFs of emission at 7.7, 10, 11.3, and 21  μm for NGC 4321 at 0.″85 (60 pc) resolution. Top: JWST images for NGC 4321 in each MIRI filter, restricted to the footprint of JWST-MUSE coverage (∼10 kpc; dashed blue). Middle: PDFs of inclination-corrected intensity from each image. The colors in the PDF map to the color bar in intensity used to display each image. Vertical dashed lines indicate the rms noise level in each filter at 0.″85. Bottom: the same PDF as in the middle row, but now with the y-axis on a logarithmic stretch to highlight features at the high-intensity end.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: A diagram illustrating the recording and target selection process during commensal observation with VLASS or other observations in on-the-fly mode. Panel (a) shows two circles representing the FoVs at the start of a recorded observation segment (black solid line) and at the end of the segment (blue dashed line). These circles are spaced one FoV width apart, as illustrated in (b), which shows the extrapolated FoV and phase center (C, in red) for the recorded segment. Panel (c) shows the stars (red) that the target selector will choose as targets for coherent beamforming. Panel (d) approximately illustrates the track along which the chosen stars will appear to “move” within the primary FoV as it passes over them.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: Images and PDFs of emission from the central 1 kpc at 7.7, 10, 11.3, and 21  μm for NGC 4321. Top: images of the central 1 kpc in NGC 4321 in each MIRI filter. Middle: pdf’s of inclination-corrected intensity from each image. The colors reflect the common color bar in intensity used to display each image. Bottom: the same PDFs as in the middle row, but now with the y-axis on a logarithmic stretch to highlight features at the high-intensity end.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: The Voyager signal detected in targeted observations conducted with COSMIC. The upchannelization and beamforming were conducted at the same resolutions in frequency and time as those of the VLASS search mode (0.2 s temporal resolution and 8 Hz frequency resolution). The top row shows the integrated spectra without Doppler correction (blue) and with Doppler correction (black). The bottom row shows the corresponding waterfall plots. The left and right columns show the sideband signals, and the middle column shows the carrier signal. The frequencies are recorded in the topocentric reference frame.
Paper: A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies
Authors: Debosmita Pathak, Adam K. Leroy, Todd A. Thompson, Laura A. Lopez, Francesco Belfiore, Médéric Boquien, Daniel A. Dale, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Erik Rosolowsky, Karin M. Sandstrom, Eva Schinnerer, Rowan Smith, Jiayi Sun, Jessica Sutter, Thomas G. Williams, Frank Bigiel, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, Ryan Chown, Eric Emsellem, Christopher M. Faesi, Kirsten L. Larson, Janice C. Lee, Sharon Meidt, Eve C. Ostriker, Lise Ramambason, Sumit K. Sarbadhicary, David A. Thilker
Figure caption: The PDFs of the galactic disk (in black) for our full sample at 21  μm. Vertical dashed lines show the rms noise levels for 21 μm at 0.″85. The PDFs at each filter show an overall distribution well fit by a lognormal (red) at lower intensity (residuals in gray), with high-intensity residuals (dashed gray) that are well fit by a power law (blue).
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: A plot of previous SETI surveys covering frequencies greater than 1 GHz. The x-axis represents the minimum detected equivalent isotropic radio power (EIRP; Siemion et al. 2013). The y-axis represents the transmitter rate (Price et al. 2020), which is indicative of the number of objects a survey observes. The COSMIC–VLASS point is based on the observations of previous epochs of the survey and the catalog of sources being used by the target selector.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: The Voyager signal detected in the raw voltage “stamp” files for each online antenna. Antenna 15 (ea15) does not show a signal because it had a cryogenic problem and therefore was not producing data. The x-axis represents frequency, zoomed around the signal carrier frequency of 8420.573 MHz (topocentric), and the y-axis represents time, with a total of 8 s of data at a 0.2 s resolution. The color scale represents the signal intensity in dB.