adsabs/AstroCLIMB huggingface dataset:
Paper: EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3
Authors: Miroslav D. Filipović, Shi Dai, Bojan Arbutina, Natasha Hurley-Walker, Robert Brose, Werner Becker, Hidetoshi Sano, Dejan Urošević, T. H. Jarrett, Andrew M. Hopkins, Rami Z. E. Alsaberi, R. Alsulami, Cristobal Bordiu, Brianna Ball, Filomena Bufano, Christopher Burger-Scheidlin, Evan Crawford, Jayanne English, Frank Haberl, Adriano Ingallinera, Anna D. Kapinska, Patrick J. Kavanagh, Bärbel S. Koribalski, Roland Kothes, Sanja Lazarević, Jonathan Mackey, Gavin Rowell, Denis Leahy, Sara Loru, Peter J. Macgregor, Luciano Nicastro, Ray P. Norris, Simone Riggi, Manami Sasaki, Milorad Stupar, Corrado Trigilio, Grazia Umana, Tessa Vernstrom, Branislav Vukotić
Figure caption: (a) Intensity distribution of H I obtained from HI4PI (HI4PI Collaboration et al. 2016). The integration velocity range is from −2.5 to 9.1 km s−1. The superposed contours indicate the intensity of the radio continuum. (b–c) Position–velocity diagrams of H I. The H I intensity is integrated from 157.°70 to 159.°15 in R.A. for panel (b) and from −65.°08 to −64.°54 in decl. for panel (c). The white dashed curve and yellow solid box in the position–velocity diagrams indicate candidates of a H I expanding shell and a high-velocity wing (see the text).
Paper: EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3
Authors: Miroslav D. Filipović, Shi Dai, Bojan Arbutina, Natasha Hurley-Walker, Robert Brose, Werner Becker, Hidetoshi Sano, Dejan Urošević, T. H. Jarrett, Andrew M. Hopkins, Rami Z. E. Alsaberi, R. Alsulami, Cristobal Bordiu, Brianna Ball, Filomena Bufano, Christopher Burger-Scheidlin, Evan Crawford, Jayanne English, Frank Haberl, Adriano Ingallinera, Anna D. Kapinska, Patrick J. Kavanagh, Bärbel S. Koribalski, Roland Kothes, Sanja Lazarević, Jonathan Mackey, Gavin Rowell, Denis Leahy, Sara Loru, Peter J. Macgregor, Luciano Nicastro, Ray P. Norris, Simone Riggi, Manami Sasaki, Milorad Stupar, Corrado Trigilio, Grazia Umana, Tessa Vernstrom, Branislav Vukotić
Figure caption: RGB image of G288.8–6.3 as seen in the eROSITA all-sky surveys eRASS:5. Photons to produce the image were color-coded according to their energy (red for energies 0.2–0.7 keV, green for 0.7–1.2 keV, blue for 1.2–2.4 keV). An adaptive kernel smoothing algorithm was applied to the images in each energy band. Radio contour lines (green: 0.1, 0.2, 0.5, and 1 mJy beam−1) are overlaid to mark the outline of G288.8–6.3. The positions of the neighboring radio pulsar PSR J1036–6559 and the Fermi source 4FG J1028.7–6431c are shown.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: Starlight-subtracted and roll-combined final JWST/NIRCam images of AU Mic in both F356W (top) and F444W (bottom). The images have been oriented such that the assumed disk major axis is parallel to the x-axis. To highlight the relative brightness of the disk at F356W, the images are displayed with the same linear color stretch. Both images have been smoothed with a σ = 0.5 pixel Gaussian for presentation and are displayed within a 10″ × 3.″5 FOV. The approximate coronagraphic inner working angle is indicated by the dashed black circle, while the approximate position of the occulted star is marked with a white star symbol.
Paper: EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3
Authors: Miroslav D. Filipović, Shi Dai, Bojan Arbutina, Natasha Hurley-Walker, Robert Brose, Werner Becker, Hidetoshi Sano, Dejan Urošević, T. H. Jarrett, Andrew M. Hopkins, Rami Z. E. Alsaberi, R. Alsulami, Cristobal Bordiu, Brianna Ball, Filomena Bufano, Christopher Burger-Scheidlin, Evan Crawford, Jayanne English, Frank Haberl, Adriano Ingallinera, Anna D. Kapinska, Patrick J. Kavanagh, Bärbel S. Koribalski, Roland Kothes, Sanja Lazarević, Jonathan Mackey, Gavin Rowell, Denis Leahy, Sara Loru, Peter J. Macgregor, Luciano Nicastro, Ray P. Norris, Simone Riggi, Manami Sasaki, Milorad Stupar, Corrado Trigilio, Grazia Umana, Tessa Vernstrom, Branislav Vukotić
Figure caption: Hα SuperCOSMOS grayscale (background-subtracted) image overlaid with ASKAP contours (0.1, 0.2, 0.5, and 1 mJy beam−1) of the Galactic SNR G288.8–6.3. Two yellow arrows indicate a possible Hα filament likely corresponding to radio emission. The area covering this image is marked in Figure 1 as the yellow rectangular box.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: For each filter (rows), the roll-averaged MCRDI final image (left), the best-fitting convolved model used as the constraint for MCRDI (middle), and the difference between the MCRDI result and the model image (right). The residuals use the same linear color stretch as the corresponding images to highlight that any differences are small compared to the total disk signal. A background source is visible in the lower left of the MCRDI images, at roughly (−1″, − 3″).
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: The mass–radius diagram for small planets. Data comes from the NASA Exoplanet Archive’s planetary systems table, as accessed on 2022 November 17 (NASA Exoplanet Archive 2022). Planets with mass and radius measurements to better than 50% and 15% fractional precision, respectively, are shown as the circles with 1σ error bars. The opacity of the points is proportional to mass measurement precision (i.e., a less-precise mass measurement translates to a more transparent marker). Color corresponds to equilibrium temperature assuming zero Bond albedo and full day–night heat redistribution. Underlying contours come from Gaussian kernel density estimation of the confirmed planets described above. The 11 transiting planets from this work are overplotted as the stars. Mass upper limits (98% confidence) are plotted for HD 25463 c (yellow star near the radius valley) and HIP 9618 c (labeled). A handful of composition curves are plotted for reference (Lopez & Fortney 2014; Zeng et al. 2016, 2019). The curves of H/He envelopes atop Earth-like cores come from Lopez & Fortney (2014) and are chosen for a planet receiving 10× Earth’s incident flux (i.e., T eq ≈ 500 K) orbiting a 10 Gyr-old, solar-metallicity star. The 50% water plus 50% Earth-like composition curve from Zeng et al. (2019) is calculated for a fixed temperature of 700 K at 100 bar, which determines the planetary model’s specific entropy. Note that familiar features of the planet radius distribution are now visible as two-dimensional features in the mass–radius plane. These include the radius valley (Fulton et al. 2017; Van Eylen et al. 2018), with center near 6 M ⊕ and 1.8 R ⊕, and the radius cliff (e.g., Kite et al. 2019), as seen by in the steep drop-off in the number of planets around 3 R ⊕.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: The same planets from Figure 10 but now plotted in terms of orbital period vs. TSM, a JWST S/N proxy (Kempton et al. 2018). Planets from the NASA Exoplanet Archive (NEA) are shown as the gray dots. Confirmed planets from the TESS-Keck Survey (TKS) are shown as the gray circles. Planets from TKS Science Case 3 (SC3), TKS’ follow-up of targets amenable to atmospheric characterization, are shown as the diamonds and stars where marker color represents host star metallicity, as measured using [Fe/H]. TKS SC3 planets from this work are the stars, where the lower limits for HD 42813 b and HIP 9618 c reflect 98% confidence. HD 25463 c is not shown because its mass constraint is too uninformative. The horizontal dashed line at TSM = 84 marks the TSM cutoff suggested by Kempton et al. (2018) for scheduling atmospheric observations of planets with 2.75 < R p < 4 R ⊕.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: Our joint modeling results for HD 25463. The figure description is the same as for Figure 6.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: The S HK portion of the joint model for HD 6061, in which GPs with some shared hyperparameters are simultaneously fit to the RVs and the Keck-HIRES S HK values. The GP kernel is described in Section 9.3. The best-fitting value of the GP period is P rot = 13.9 ± 1.5 days. See Figure 23 for the photometry and RV portions of this joint model. The GP posterior prediction is shown as the blue line surrounded by a 1σ error envelope. The Keck-HIRES S HK values are shown as the black points with 1σ errors, where the measurement error on each S HK value has been added in quadrature with the a jitter term that has been fit to the data. Residuals are shown in the bottom panel.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: Inferred values of f env as a function of planet radius for the 11 transiting planets. f env values are estimated by applying smint to the grid of thermal evolution from LF14. Several slices of the LF14 grid are plotted for reference. Color corresponds to instellation flux in Earth units. An upper limit (which reflects 98% confidence) is shown for HD 25463 c, whose actual instellation (S p ≈1400 S ⊕) surpasses the upper limit of the LF14 grid (S p =1000 S ⊕).
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: GLS periodograms for HD 25463. The figure description is the same as for Figure 7.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: GLS periodograms for HD 42813. The figure description is the same as for Figure 7.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: Our joint modeling results for HD 42813. The figure description is the same as for Figure 6.
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: Our joint modeling results for TOI-669. The figure description is the same as for Figure 6.
Paper: Measuring the Temperature of Starspots from Multi-filter Photometry
Authors: Maria C. Schutte, Leslie Hebb, John P. Wisniewski, Caleb I. Cañas, Jessica E. Libby-Roberts, Andrea S. J. Lin, Paul Robertson, Gumundur Stefánsson
Figure caption: Data for calculated HAT-P-11 contrast vs. spot temperature for the following filters are shown as data points with dashed lines: SDSS ﹩{g}^{{\prime} }﹩ (blue), SDSS ﹩{r}^{{\prime} }﹩ (magenta), SDSS ﹩{i}^{{\prime} }﹩ (red), SDSS ﹩{z}^{{\prime} }﹩ (cyan), TESS (orange), Kepler (green), and OAO Zs (black). Two polynomial fits are shown for the SDSS ﹩{r}^{{\prime} }﹩ and SDSS ﹩{i}^{{\prime} }﹩ as solid colored lines.
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: NEID Telescope fiberhead. (a) Image showing the fiberhead, with a black coating to reduce backscatter. (b) Schematic of the fiberhead adapted from Roy et al. (2020) showing the relative positions of the science and sky fiber with respect to the Coherent Fiber Bundles. (c) High-resolution image taken of the fiberhead installed in NEID, taken using a Zygo Optical profilometer. Oct 1 is the Science fiber and Oct 4 is the Sky fiber, while the other octagonal fibers are spares.
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: NEID v-groove block with the five fibers (three HR + two HE) in the process of alignment to the ball lenses during commissioning at WIYN. The yellow arrows point to the two HE fibers and ball lenses, while the red ones indicate the three HR fibers and lenses, with one of them lit up with an alignment laser. We ground the stainless steel block to prevent electrostatic discharges from disturbing the tiny lenses, and use Kapton tape and epoxy to fix the fibers in place upon alignment. This block is then capped with a foam-covered lid that is not shown in this image.
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: (a) Laser frequency comb time series with the modal-noise agitator on and off sequences interspersed by agitator movement to mix the fiber modes. Given our finite sample size and photon noise, we consider the rms difference between the two agitator cases, on (green circles) and off (red squares), to be similar. (b) Comparison of the ratio of rms scatter to the photon noise across each order index (0 is for the bluer wavelengths, and 55 toward the redder wavelengths), and do not see any chromatic trends suggestive of the λ 2 dependence of modal noise.
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: (a) Stitched collection of individual frames using the weighted averages algorithm, showing the stitch boundaries. This was later replaced by the “High Contrast” algorithm to stitch the images together. The fiberhead is 4 mm in diameter. (b) Thorlabs polka-dot pattern showing the offsets due to the imperfect stitching. Each dot is 125 μm in diameter.
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: Fiber transmission comparison for the FBP fiber used for NEID, vs. the low and high OH- variants, for 35 m length (the approximate length of the NEID fiber train).
Paper: Stable Fiber-illumination for Extremely Precise Radial Velocities with NEID
Authors: Shubham Kanodia, Andrea S. J. Lin, Emily Lubar, Samuel Halverson, Suvrath Mahadevan, Chad F. Bender, Sarah E. Logsdon, Lawrence W. Ramsey, Joe P. Ninan, Gumundur Stefánsson, Andrew Monson, Christian Schwab, Arpita Roy, Leonardo A. Paredes, Eli Golub, Jesus Higuera, Jessica Klusmeyer, William McBride, Cullen Blake, Scott A. Diddams, Fabien Grisé, Arvind F. Gupta, Fred Hearty, Michael W. McElwain, Jayadev Rajagopal, Paul Robertson, Ryan C. Terrien
Figure caption: Schematic of the NEID fiber train for the High Resolution Science fiber (not to scale).