adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for Planets Orbiting Vega with the James Webb Space Telescope
Authors: Charles Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Marie Ygouf, Alexandra Greenbaum, Jarron Leisenring, Andras Gaspar, John Krist, George Rieke, Schuyler Wolff, Kate Su, Klaus Hodapp, Michael Meyer, Doug Kelly, Martha Boyer, Doug Johnstone, Scott Horner, Marcia Rieke
Figure caption: The three JWST data points (one NIRCam and two MIRI) for the source S1 are compared with illustrative SEDs of a number of extragalactic objects (from a suite of Spitzer SWIRE templates; M. Polletta et al. 2007) and with the spectrum of cloudless T eff = 200 K, log (g) = 3 Sonora Bobcat model (M. S. Marley et al. 2021).
Paper: Searching for Planets Orbiting Vega with the James Webb Space Telescope
Authors: Charles Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Marie Ygouf, Alexandra Greenbaum, Jarron Leisenring, Andras Gaspar, John Krist, George Rieke, Schuyler Wolff, Kate Su, Klaus Hodapp, Michael Meyer, Doug Kelly, Martha Boyer, Doug Johnstone, Scott Horner, Marcia Rieke
Figure caption: The planet occurrence rate for a planet in two separation ranges (10–100 au (black) and 50–100 au (blue)), as a function of the lower-mass cutoff, M min, integrated up to to 13 M J, following the formulation of Equation (2). The E. L. Nielsen et al. (2019) occurrence rate of 8.9% (10–100 au, 5–13 M J) is indicated as a black data point while the predicted occurrence rate of ∼30% at the NIRCam sensitivity level of 0.5–13 M J for 50–100 au is indicated by the blue data point. The yellow shaded regions surrounding each line denote the ±1σ uncertainty due to the uncertainty in the the value of the nominal occurrence rate, f.
Paper: Searching for Planets Orbiting Vega with the James Webb Space Telescope
Authors: Charles Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Marie Ygouf, Alexandra Greenbaum, Jarron Leisenring, Andras Gaspar, John Krist, George Rieke, Schuyler Wolff, Kate Su, Klaus Hodapp, Michael Meyer, Doug Kelly, Martha Boyer, Doug Johnstone, Scott Horner, Marcia Rieke
Figure caption: The figure shows the combined effects of the proper motion and parallax of Vega as a function of time since NIRCam’s initial observation on 2023 August 19. The initial epoch and two future epochs within JWST’s availability window are marked. Even a year after these initial observations the position offset relative to the initial observation will be >250 mas and easily detectable.
Paper: Searching for Planets Orbiting Vega with the James Webb Space Telescope
Authors: Charles Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Marie Ygouf, Alexandra Greenbaum, Jarron Leisenring, Andras Gaspar, John Krist, George Rieke, Schuyler Wolff, Kate Su, Klaus Hodapp, Michael Meyer, Doug Kelly, Martha Boyer, Doug Johnstone, Scott Horner, Marcia Rieke
Figure caption: (left) NIRCam subarray PCA reduction at F444W showing the source S1 at ∼2 o’clock. (Center and right) MIRI observations optimized for point-source detection identifies the same source at F1550 and F2550W, strongly suggesting this object is extragalactic in nature (K. Y. L. Su et al. 2024, in preparation). In all three images intensity units are MJy sr−1.
Paper: Searching for Planets Orbiting Vega with the James Webb Space Telescope
Authors: Charles Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Marie Ygouf, Alexandra Greenbaum, Jarron Leisenring, Andras Gaspar, John Krist, George Rieke, Schuyler Wolff, Kate Su, Klaus Hodapp, Michael Meyer, Doug Kelly, Martha Boyer, Doug Johnstone, Scott Horner, Marcia Rieke
Figure caption: PSF-subtracted images of the subarray data. The bright residuals are residuals from the imperfectly subtracted speckles. The northeast part of the F210M data (right) is missing due to the PSF falling close to the southwest detector gap, i.e., the edge of NIRCam detector A2.
Paper: Searching for Planets Orbiting Vega with the James Webb Space Telescope
Authors: Charles Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Marie Ygouf, Alexandra Greenbaum, Jarron Leisenring, Andras Gaspar, John Krist, George Rieke, Schuyler Wolff, Kate Su, Klaus Hodapp, Michael Meyer, Doug Kelly, Martha Boyer, Doug Johnstone, Scott Horner, Marcia Rieke
Figure caption: NIRCam subarray PCA reduction at F444W shows two sources, S1 and S2, are both extended. Two different stretches of the reduced image are superimposed to emphasize the sources; the color bar is applicable to the inner region only. Details of the analysis are presented in the Appendix.
Paper: Preparing for the Early eVolution Explorer: Characterizing the Photochemical Inputs and Transit Detection Efficiencies of Young Planets Using Multiwavelength Flare Observations by TESS and Swift
Authors: Ward S. Howard, Meredith A. MacGregor, Adina D. Feinstein, Laura D. Vega, Ann Marie Cody, Neal J. Turner, Valerie J. Scott, Jennifer A. Burt, Laura Venuti
Figure caption: Simultaneous 20 s cadence Swift NUV and TESS light-curve segments, stitched together to create a time series of 0.6 day. Top panel: the NUV light curve is shown with fluxes and uncertainties adjusted to the photometric uncertainty for the count rate of the faintest star in the sample. Times where the flare decay was not observed are simulated by fitting a flare tail to the observed flux times and shown in gray. The fit to the flares is shown in cyan. Middle panel: the simultaneous data in the stitched TESS light curve are shown with fluxes and uncertainties adjusted to the TESS magnitude of the faintest star in the sample, AP Col. Small sympathetic peaks during the decay phase of the largest TESS flares are subtracted from the light curve when they occur during the synthetic times in the NUV light curve. This is because they could not have been predicted in principle and would therefore bias the analysis. The model prediction is shown in orange, where the tTESS and σTESS parameters have been allowed to vary by 30 s and 10%, respectively. Bottom panel: the residual TESS light curve after subtracting the model of the predicted behavior of the TESS light curve.
Paper: Preparing for the Early eVolution Explorer: Characterizing the Photochemical Inputs and Transit Detection Efficiencies of Young Planets Using Multiwavelength Flare Observations by TESS and Swift
Authors: Ward S. Howard, Meredith A. MacGregor, Adina D. Feinstein, Laura D. Vega, Ann Marie Cody, Neal J. Turner, Valerie J. Scott, Jennifer A. Burt, Laura Venuti
Figure caption: Simultaneous EVE observations of large flares will discriminate between constant UV/optical ratios and UV/optical ratios that increase with energy. The current literature sample of simultaneous detections from R. R. Paudel et al. (2024) is composed of smaller flares, while EVE is sensitive to some of the largest flares emitted by young stars. The EVE samples for constant and increasing Teff–energy scenarios are drawn from the FFD and flare yield predictions of Section 6. The right y-axis shows the surface mixing ratio of O2 in an Earth-like atmosphere resulting from photochemistry, where we assume for purposes of illustration that the flare Teff that produces the observed NUV/TESS ratio can be used to estimate a FUV/NUV ratio. At the largest energies, excess UV emission corresponds to an increase of 30–60× in abiotic O2 production for Earth-like atmospheres (C. E. Harman et al. 2015).
Paper: Preparing for the Early eVolution Explorer: Characterizing the Photochemical Inputs and Transit Detection Efficiencies of Young Planets Using Multiwavelength Flare Observations by TESS and Swift
Authors: Ward S. Howard, Meredith A. MacGregor, Adina D. Feinstein, Laura D. Vega, Ann Marie Cody, Neal J. Turner, Valerie J. Scott, Jennifer A. Burt, Laura Venuti
Figure caption: Multiwavelength flare yield estimates for a 2 yr science mission, with conservative assumptions of 50% science margin and 9% NUV throughput. The FOV plot assumes 0.1 e− s−1 and a read noise 4 e−1. Flares are detected at 3σ. This figure is intended to illustrate how large differences in flare yields can arise when varying the instrument parameters across a reasonable range of values, and is not intended to specify the final instrument design of EVE. Other sets of instrument parameters are possible (e.g., increased transmission, quantum efficiency, or aperture), but this study demonstrates acceptable flare yields are achieved for feasible instrument designs.
Paper: Preparing for the Early eVolution Explorer: Characterizing the Photochemical Inputs and Transit Detection Efficiencies of Young Planets Using Multiwavelength Flare Observations by TESS and Swift
Authors: Ward S. Howard, Meredith A. MacGregor, Adina D. Feinstein, Laura D. Vega, Ann Marie Cody, Neal J. Turner, Valerie J. Scott, Jennifer A. Burt, Laura Venuti
Figure caption: Left panel: the number of flares needed to reject the ∼9000 K energy budget null hypothesis at a given confidence level using an A-D test. Curves are shown for a range of cadences, where each curve represents a 3σ confidence interval on the distribution of p-values measured from a sample size of Nflares. Right panel: the number of flares needed to ensure the observed FFD power-law slope αFFD is representative of the true average flare rate in both the NUV and optical bands. This is the number of flares needed to reject the null hypothesis of αFFD ≈ 1.6, and is insensitive to cadences of 20–120 s.
Paper: Preparing for the Early eVolution Explorer: Characterizing the Photochemical Inputs and Transit Detection Efficiencies of Young Planets Using Multiwavelength Flare Observations by TESS and Swift
Authors: Ward S. Howard, Meredith A. MacGregor, Adina D. Feinstein, Laura D. Vega, Ann Marie Cody, Neal J. Turner, Valerie J. Scott, Jennifer A. Burt, Laura Venuti
Figure caption: Left panel: flare energies in the TESS and NUV bands during the flare peak. Lines representing flare energy budgets for the 9000 K scenario and the NUV-luminous prediction from J. A. G. Jackman (2022) are shown for reference. The best-fit scaling relationship to the observed sample is shown in red. Right panel: predicted time lags between the initial NUV flare peaks and the subsequent TESS band flare peaks. Predicted peak times in the TESS band are determined using the centroid of the second time integral of the flare model fit to the NUV light curves.
Paper: Preparing for the Early eVolution Explorer: Characterizing the Photochemical Inputs and Transit Detection Efficiencies of Young Planets Using Multiwavelength Flare Observations by TESS and Swift
Authors: Ward S. Howard, Meredith A. MacGregor, Adina D. Feinstein, Laura D. Vega, Ann Marie Cody, Neal J. Turner, Valerie J. Scott, Jennifer A. Burt, Laura Venuti
Figure caption: Left panel: transit detection efficiency for a T = 9.64 star after flare detrending computed from 10,000 planet injection and recovery trials. The grayscale grid is the fraction of transits recovered in each planet period and transit depth bin, with lighter shades representing higher detection fractions. The 50% detection threshold with detrending is highlighted in cyan, while the 50% detection threshold in the case of no flare detrending is shown in magenta for comparison. Overplotted are simulated planets, with a color map representing their S/N in the BLS periodogram. Right panel: same as the left panel for the no-flare-detrending scenario. The flare detrending process increases the transit depth δ by Δδ = 0.0052, which corresponds to an increase of 0.42R⊕ for a K7V star.
Paper: Preparing for the Early eVolution Explorer: Characterizing the Photochemical Inputs and Transit Detection Efficiencies of Young Planets Using Multiwavelength Flare Observations by TESS and Swift
Authors: Ward S. Howard, Meredith A. MacGregor, Adina D. Feinstein, Laura D. Vega, Ann Marie Cody, Neal J. Turner, Valerie J. Scott, Jennifer A. Burt, Laura Venuti
Figure caption: Examples of 5 × 5 deg2 cluster pointings that produce high yields of simultaneous NUV flare detections. Here, we show the core region with the highest flare yield per cluster even though some clusters have multiple high-yield core regions.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: Pixel latency time (in seconds, left scale) across the TANDEM CMOS detector for objects in motion according to different dynamical environments. Latency time directly reflects into a magnitude threshold for object detection (right scale), through Equation (13). In particular, the SST domain includes Earth-orbiting artificial satellites and space debris (both in prograde and retrograde motion, respectively, red and green coded in the plot) at the different orbital regimes, namely low-, medium-Earth, and geostationary orbits (see, e.g., B. Pattan 1993, for details), up to the circumterrestrial outer edge at about 35,786 km. Due to their special nature, SST observations are typically carried out with telescope sidereal tracking “off” (see A. Buzzoni 2024a, for further insights upon SST observing strategies). Magnitude threshold for deep-space objects, at the Moon distance and beyond, as marked, is accounted for by the magenta curve. Detection limits for even farther solar system objects, at increasing planetary distance, are finally accounted for by the blue curve, which also includes the illustrative TANDEM detection threshold for main-belt asteroids. These observations usually require a more standard astronomical approach, with sidereal tracking “on,” as labeled on the plot.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: Astrometric accuracy of the four TANDEM telescopes (coded with T1, T2, T3, and T4 in the plots) across a 2° × 2° dense stellar field around the A. U. Landolt (1992) standard PG1528+062. Each panel maps the 4096 × 4096 pixel GSense 4040 image. Plate solutions were obtained independently for each telescope by relying on the Astrometrica + Gaia DR2 catalog, as a reference. Star size in the plots is proportional to the astrometric uncertainty. As summarized in the central legend inset, orange dots are stars with an astrometric accuracy of 0.1″ or better, yellow dots are for 0.1″–0.2″, cyan dots are for the 0.2″–0.4″ range, pale blue dots are for 0.4″–1﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩0″ residuals, and finally dark blue dots are for stars displaying astrometric residuals in excess of 1″.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: According to Equation (13), solid lines display the magnitude limit for an S/N = 3 detection threshold in the different photometric bands (as reported in the legend on the plot) reached by each TANDEM telescope with increasing exposure time. The corresponding saturation cap is also showed (dashed lines) according to Equation (12).
Paper: Origins of Super Jupiters: TOI-2145b has a Moderately Eccentric and Nearly Aligned Orbit
Authors: Jiayin Dong, Ashley Chontos, George Zhou, Gudmundur Stefansson, Songhu Wang, Chelsea X. Huang, Arvind F. Gupta, Samuel Halverson, Shubham Kanodia, Jacob K. Luhn, Suvrath Mahadevan, Andrew Monson, Jaime A. Alvarado-Montes, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: NEID’s first RM-effect visit on 2023 May 26. Data were reduced by three different reduction techniques. The inferred projected stellar obliquities are consistent, but DT provides the tightest constraint. (a) and (b) In-transit RV measurements of the TOI-2145 system using the NEID spectra. The blue dots and black bars are NEID RVs and their corresponding uncertainties. The planet’s transit and midtransit time are indicated by the gray shaded region and gray vertical line, respectively. (c) The DT (planetary shadow) signal of the TOI-2145 system during TOI-2145b’s transit. The left, middle, and right panels are data extracted from the NEID spectra, best-fit model, and the residual of the data after subtracting the best-fit model, respectively. The color scale presents the flux variation of the velocity channel.
Paper: Origins of Super Jupiters: TOI-2145b has a Moderately Eccentric and Nearly Aligned Orbit
Authors: Jiayin Dong, Ashley Chontos, George Zhou, Gudmundur Stefansson, Songhu Wang, Chelsea X. Huang, Arvind F. Gupta, Samuel Halverson, Shubham Kanodia, Jacob K. Luhn, Suvrath Mahadevan, Andrew Monson, Jaime A. Alvarado-Montes, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: TTV on TOI-2145b. The planet exhibits a TTV of less than 5 minutes over a 4 yr baseline, with a typical midtransit time uncertainty of 2.7 minutes.
Paper: Searching for Planets Orbiting Vega with the James Webb Space Telescope
Authors: Charles Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Marie Ygouf, Alexandra Greenbaum, Jarron Leisenring, Andras Gaspar, John Krist, George Rieke, Schuyler Wolff, Kate Su, Klaus Hodapp, Michael Meyer, Doug Kelly, Martha Boyer, Doug Johnstone, Scott Horner, Marcia Rieke
Figure caption: (Top) MCMC analysis of the F444W source S1 located at roughly the 2 o’clock position and 6″ away from Vega (Table 3, Figure 4). (Bottom) MCMC analysis of the F444W S2 source located at roughly the 11 o’clock position and 6″ away from Vega. This source appears to be slightly extended.
Paper: Searching for Planets Orbiting Vega with the James Webb Space Telescope
Authors: Charles Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Marie Ygouf, Alexandra Greenbaum, Jarron Leisenring, Andras Gaspar, John Krist, George Rieke, Schuyler Wolff, Kate Su, Klaus Hodapp, Michael Meyer, Doug Kelly, Martha Boyer, Doug Johnstone, Scott Horner, Marcia Rieke
Figure caption: (Top) An inset from Figure 4 shows the position of the marginal detection discussed in this appendix. (Bottom) MCMC analysis of the F444W source S3 approximately 1.″4 due south of Vega (Table 3).
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: MCMC corner plot for the triple-star system Gaia DR3 249662295687401216. The fitted model parameters are: for the inner binary: q1 = 0.919 ± 0.006, ﹩{K}_{1}=138.79{8}_{-0.749}^{+0.727}﹩, ﹩\sqrt{{e}_{1}}\cos {\omega }_{1}=0﹩, ﹩\sqrt{{e}_{1}}\sin {\omega }_{1}=0.0014\pm 0.001﹩; outer binary: ﹩\sqrt{{e}_{2}}\cos {\omega }_{2}=-0.00{8}_{-0.008}^{+0.015}﹩, ﹩\sqrt{{e}_{2}}\sin {\omega }_{2}=0.14{4}_{-0.068}^{+0.085}﹩, ﹩{q}_{2}=\mathrm{0.0.42}{7}_{-0.068}^{+0.077}﹩, ﹩{K}_{3}=21.27{5}_{-1.484}^{+1.752}﹩; and the system velocity: ﹩\gamma =7.7{4}_{-0.988}^{+1.038}\,\,{\rm{km s}}^{-1}\,﹩.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: RV fitting for the triple-star system Gaia DR3 2077667962475652864.The black points and red stars represent the observed data after phase folding, and the red line indicates the fitted RV curve. The blue points show the velocity of the inner binary's center of mass, while the green dashed line represents the fitted curve for the inner binary's center of mass velocity. The green points indicate the velocity of the tertiary star, and the green dashed line illustrates the fitted curve for the tertiary star's velocity. V1 and V2 denote the RVs of the primary and secondary stars in the inner binary, respectively, and V3 represents the RV curve of the tertiary star.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: The MCMC corner plot for the triple-star system Gaia DR3 249662295687401216. The fitted model includes the binary parameters (inclination incl i, temperature ratio T2/T1, R1/a, R2/a) and the third light fraction L3.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: MCMC corner plot for the triple-star system Gaia DR3 2077667962475652864. The fitted model parameters are: for the inner binary, q1 = 0.937 ± 0.003, ﹩{K}_{1}=91.97{1}_{-0.153}^{+0.160}﹩, ﹩{\sqrt{e}}_{1}\cos {\omega }_{1}=0﹩, ﹩{\sqrt{e}}_{1}\sin {\omega }_{1}=0.009\pm 0.001﹩; for the outer binary: ﹩{\sqrt{e}}_{2}\cos {\omega }_{2}=0.02{8}_{-0.0}^{+0.001}﹩, ﹩{\sqrt{e}}_{2}\sin {\omega }_{2}=-0.293\pm 0.001﹩, q2 = 0.393 ± 0.003, ﹩{K}_{3}=30.00{1}_{-0.047}^{+0.049}﹩; and the systemic velocity ﹩\gamma =4.58{2}_{-0.025}^{+0.023}﹩ km s−1.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: The MCMC corner plot for the triple system j03, representing the results of inner orbital fitting. The fitted parameters are: ﹩{q}_{1}=0.60{0}_{-0.009}^{+0.008}﹩, ﹩{K}_{1}=96.69{3}_{-0.610}^{+0.615}﹩, ﹩\sqrt{{e}_{1}}\cos {\omega }_{1}=0.001﹩, ﹩\sqrt{{e}_{1}}\sin {\omega }_{1}=-0.03{2}_{-0.006}^{+0.005}﹩, and the systemic velocity ﹩\gamma =14.53{8}_{-0.311}^{+0.322}﹩ km s−1.
Paper: Identifying Hierarchically Triple Star Systems with Gaia DR3 and LAMOST
Authors: Tongyu He, Jiao Li, Jiangdan Li, Jianping Xiong, Xiaobin Zhang, Mikhail Kovalev, Qiyuan Cheng, Sufen Guo, Mingkuan Yang, Xuefei Chen, Zhanwen Han
Figure caption: Light curve of the triple Gaia DR3 2077667962475652864. The blue dots indicate phase-folded observations, and the solid yellow line indicates the results of the fit. The horizontal axis indicates the phase, and the fitting residuals are shown at the bottom of the plot.
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: Spatial coverage of observations. In this study, we rely on Plateau de Bure Interferometer (PdBI), Northern Extended Millimeter Array (NOEMA), and Submillimeter Array (SMA) observations, each of which covered some extent of the disk of M51. The boxes indicate which lines were observed by each respective program. Background HST image credit: NASA, ESA, S. Beckwith (STScI), and The Hubble Heritage Team (STScI/AURA).