adsabs/AstroCLIMB huggingface dataset:
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: Short-spacing correction analysis. The top panels show the 12CO(2–1) (top-left panel) and 13CO(2–1) (top-right panel) spectra, averaged over the entire FOV. We obtain the red spectrum when using only the SMA SUB+COM cube. After short-spacing correction (SMA+IRAM), we obtain the blue spectrum. For 12CO(2–1), it is evident that half of the emission is missing in the interferometric data. The lower panels show the amplitudes in the overlapping uv space of the IRAM and SMA data (ranging from 13″–28″) ratio of the amplitudes (bottom-left panel), and the amplitude distribution (bottom-right panel) for the high- (SMA) and low- (IRAM 30 m) resolution data separately.
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: Deriving an estimate for the dust-to-gas ratio (DGR). The background illustrates the 12CO(1–0) moment-0 map at 4″. The larger hexagonal grid indicates the map from J. S. den Brok et al. (2023b) for which we have HI and dust mass measurements (at 26″ resolution). For the blue marked hexagons, we have non-LTE α CO values for >70% in terms of the total 12CO(1–0) intensity from within that pixel.
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: Correlation of LTE and non-LTE parameters. Each box represents the strength of the LTE or non-LTE-derived parameters (on the x-axis) with some key observables or galactic parameters (on the y-axis). We note that we have scaled the non-LTE 12CO column density by the beam filling factor. Red indicates a positive correlation, and blue indicates a negative correlation. The correlation is quantified by the Kendall’s τ correlation coefficient. The size of the points indicates the inverse p value (larger points show a significant correlation with p < 0.05). Strong correlations, where ∣τ∣ > 0.5, are indicated by hatched markers.
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: Significant (5σ) line ratio detection. Each panels illustrates the sight lines per line ratio for which both lines are significantly detected at S/N > 5 by the red contour. For reference, each panel also lists the number of sight lines and the percentage of 12CO(1–0) flux contained for the selected sight lines in the top-left corner. The sight lines are colored by the CO(1–0) moment-0 to show M51's morphology.
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: Although flare rates and energies are measured in the optical for most stars, the FUV and NUV energies determine the photochemical radiation environment of orbiting planets during these events. Simultaneous observations at UV and optical wavelengths are needed to derive the energy budget as flares with similar emission levels at optical wavelengths can produce NUV fluxes that differ by 2–20× depending on the Teff of the flare, correlating with order-of-magnitude discrepancies at FUV wavelengths. Spectra of ϵ Eri during the two flares are obtained by superimposing the flare blackbody onto the semi-empirical base spectrum from P. R. Behr et al. (2023).
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: Predicted times for representative TESS band light curves relative to the times of the NUV peaks (which occur at t = 0 on the x-axis and are not otherwise shown). A one- or two-component Gaussian is fit to the peak of the NUV light curve and the double time integral is computed, shown for reference here in salmon. The predicted time of the TESS peak is then given as the time compared to the NUV peak.
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: NUV 22 s cadence light curves of the 13 flares meeting our detection criteria. Flares are ordered by host star and size. The 5σ detection threshold is shown as a black dashed line, and times with simulated light-curve data during gaps caused by the Swift duty cycle are shown in gray. Simulated sections are produced by fitting the G. Tovar Mendoza et al. (2022) flare model to the observed part of the decay phase and varying the points within the expected photometric uncertainties. The flare peak is fully covered by the Swift observations during 12 flares and partially covered during one flare (EV Lac F3).
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 TESS light curves of the 13 flares meeting our detection criteria. The TESS components of the flares are ordered and displayed on the same time axis as in Figure 2. The local flux baseline determined from the average of the nearby out-of-flare points is shown as a black solid line, and the uncertainty in this baseline value is shown in gray. The 3σ detection threshold relative to this value is shown as a black dashed line.
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: Top panels: simultaneous 20 s cadence light curves of the G 41-14 F1 and GJ 674 F1 events. Although the NUV light curves of both flares are clearly visible, the significance of the TESS light curve of GJ 674 F1 appears much weaker than that of G 41-14 and would have been missed at a lower cadence. The y-axis of the GJ 674 plot has been scaled by the ratio of the TESS to NUV flux amplitude for the G 41-14 flare in order to show the lower TESS-to-NUV flux ratio of the GJ 674 flare. Bottom panels: same as the top panels, but for the EV Lac F1 and G 41-14 F3 events. Although the TESS band energies of the flares are comparable, the NUV energy of the EV Lac flare is 2.4× higher than that of the G 41-14 flare.
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: Predicted shapes for representative TESS band light curves based on the single time integral of the model fit to the corresponding NUV light curve. The predicted shapes are a superposition of the separate component peaks, and the resulting complex flare model’s time axis is adjusted by the time lag shown in Figure 4. The flare amplitude of each component is left free to fit to the TESS flux variability and is not a prediction.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Left: temperature–pressure profile of HD 189733b inferred from NIRCam emission spectra (red), compared with that inferred from HST and Spitzer emission spectra (black). Right: the emission spectrum used to infer the T/P profile, converted to brightness temperature. The gray bands indicate the bandpasses of Spitzer/IRAC channels 1 and 2, which overlap with the NIRCam data. At a given wavelength, the brightness temperature is roughly the temperature of the photosphere. It can be compared to 1540 K, the temperature of a zero albedo, zero heat redistribution blackbody at HD 189733b’s semimajor axis.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Difference in expected log predicted density between the reference retrieval on HD 189733b (with a power-law haze and no methane depletion) and an alternate retrieval. The alternate retrievals have C/O fixed to 0.1 (upper left), or the opacity of one molecule zeroed out (upper right: CO; lower left: H2S; lower right: CO2).
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Comparison between the adjusted gas-phase metallicity and C/O inferred from the equilibrium retrieval (black) and the free retrieval (red), for transit (left) and eclipse (right).
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: JWST transmission spectra of HD 189733b compared to that of two other hot Jupiters, all normalized by scale height. HD 209458b and 189733b data are from NIRCam, while WASP-39b data are from PRISM.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Posteriors for the fiducial NIRCam transmission spectrum retrieval, which assumes equilibrium chemistry with methane depletion.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Posteriors for the fiducial NIRCam emission spectrum retrieval, which assumes equilibrium chemistry without methane depletion.
Paper: frb-voe: A Real-time Virtual Observatory Event Alert Service for Fast Radio Bursts
Authors: Thomas C. Abbott, Andrew V. Zwaniga, Charanjot Brar, Victoria M. Kaspi, Emily Petroff, Mohit Bhardwaj, P. J. Boyle, Amanda M. Cook, Ronniy C. Joseph, Kiyoshi W. Masui, Ayush Pandhi, Ziggy Pleunis, Paul Scholz, Kaitlyn Shin, Shriharsh Tendulkar
Figure caption: Workflow for the FRB alert service. Observatories that detect FRBs in real-time or post real-time (e.g., archival searches) can make equal use of this workflow. From left to right: (upper) a burst is detected at the host observatory, either a new FRB or a burst from a known repeating FRB or (lower) the frb-voe service’s operator initiates a retraction or update VOEvent. The metadata are sent to the frb-voe server via requests and then saved to the MongoDB database. Optionally, the frb-voe server can request a TNS name. Finally, after validating the data, the server broadcasts email and machine-readable XML alerts to subscribers and automated follow-up observatories. Icons from The Noun Project (see acknowledgments for complete list of creators).
Paper: Faint White Dwarf Flux Standards: Data and Models
Authors: Ralph C. Bohlin, Susana Deustua, Gautham Narayan, Abhijit Saha, Annalisa Calamida, Karl D. Gordon, Jay B. Holberg, Ivan Hubeny, Thomas Matheson, Armin Rest
Figure caption: Model fit and residuals for WDFS1434-28 with the parameters from Table 4 written on the plot. The heavy red line in the top two panels represents the model divided by its continuum to flatten the display and preserve spectral features, while in all three panels, the residuals are large green circles for the WFC3 photometry, large purple circles for the useful STIS bins, and a large black circle for the STIS G140L bin that is not used as a constraint to the fit. Middle panel: small diamonds are STIS data for G140 (red) and G230L (black). The dip in the model near 1400 Å is a quasi-molecular hydrogen feature. Bottom panel: the purple bars that indicate the bin width and the black circle are omitted for clarity. The red and black STIS data are binned to a resolution R = 500.
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: Two views of the TANDEM telescope array, on top of its rotating arm, in a piggyback mounting at the decl. axis flange of the Cassini main telescope (behind in the left picture). TANDEM telescopes share Cassini's polar axis maneuvering, while moving the combination independently in decl. In addition, each of the telescopes is allowed a supplementary and independent steering by ±10° around the common pointing direction (both R.A. and decl.) by means of individual tilt/spin actuators on board (visible in the right picture).
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: The “first light” of TANDEM, just after the preliminary focusing operations on 2023 June 28. A spectacular B-band image of the waxing gibbous Moon is taken with the shortest exposure time allowed by the electronic shutter on board the CMOS, namely just 0.02 ms.
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: The optical design of the TANDEM telescopes. Each instrument is a customized ORION AG14 telescope with a 35 cm aperture diameter and Newtonian design, carried to a focal ratio f/3 and coupled with an ad hoc 4″ Wynne field corrector. Imagery is provided through a Moravian C4-16000 camera mounting a Johnson–Cousins BVRI filter wheel and a CMOS GSense 4040 (4096 × 4096 pixels with 9 μm pixel size).
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: The ADS concept for TANDEM, as approved for final assembly in summer 2022. Note in the sketch the four telescopes (in black) mounted on a rotating arm (in blue) anchored orthogonally to the Cassini (in green) polar axis (in yellow).
Paper: 5 cm OH Masers in Northern Star Formation Regions
Authors: Hai-Hua Qiao, Xu-Jia Ouyang, Zhi-Qiang Shen, Shari L. Breen, Kai Yang, Xi Chen, Juan Li
Figure caption: The distribution of OH maser sites with magnetic field direction measurements in the Galaxy. The magnetic field direction data set derived from Zeeman splitting includes our results from 6.0 GHz excited-state OH masers (blue circles and red crosses), as well as ground-state (J. A. Green et al. 2012b) and 6.0 GHz excited-state (J. A. Green et al. 2015; X.-J. Ouyang et al. 2022) OH maser magnetic field results (blue diamonds and red pluses). Red symbols represent sources with a positive magnetic field direction, whereas blue symbols represent sources with a negative magnetic field direction. The background image of the Galaxy is from Xing-Wu Zheng & Mark Reid BeSSeL/NJU/CFA. The yellow circle indicates the position of the Sun, and the black dot marks the center of the Galaxy.
Paper: 5 cm OH Masers in Northern Star Formation Regions
Authors: Hai-Hua Qiao, Xu-Jia Ouyang, Zhi-Qiang Shen, Shari L. Breen, Kai Yang, Xi Chen, Juan Li
Figure caption: Panel (a): detection rate of each OH transition at 6.0 GHz toward 155 target sources; Panel (b): association rates between 6030/6035 MHz OH masers and methanol/water masers.
Paper: 5 cm OH Masers in Northern Star Formation Regions
Authors: Hai-Hua Qiao, Xu-Jia Ouyang, Zhi-Qiang Shen, Shari L. Breen, Kai Yang, Xi Chen, Juan Li
Figure caption: The 6030, 6035, and 6049 MHz OH spectra toward G133.947+1.064 (W3(OH)). The x-axis shows the radial velocity (with respect to the LSR) in units of km s−1, and the y-axis is Stokes I, the total flux density in units of Jy.
Paper: 5 cm OH Masers in Northern Star Formation Regions
Authors: Hai-Hua Qiao, Xu-Jia Ouyang, Zhi-Qiang Shen, Shari L. Breen, Kai Yang, Xi Chen, Juan Li
Figure caption: The relation of the LHC and RHC polarization peak flux densities of the 6030 and 6035 MHz OH masers in 13 6.0 GHz OH maser sources. The solid line represents the peak flux density of the 6035 MHz OH maser, which is equal to that of the 6030 MHz OH maser. The dotted line indicates the peak flux density of the 6035 MHz OH maser is 10 times that of the 6030 MHz OH maser. The dashed line illustrates the peak flux density of the 6035 MHz OH maser is 100 times that of the 6030 MHz OH maser.
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: our detection limits are shown for each filter (F210M and F444W) as a function of separation from the parent star, in terms of contrast ratio (right-side axis) and apparent magnitude (left-side axis). The drop in detectability at ∼9″ corresponds to the boundary between subarray and full-frame imaging. The limits are given as 5σ. The pre-JWST contrast limit at M band from Keck (B. B. Ren et al. 2023) is shown as a dashed line for comparison; the JWST detections limits are a factor of ∼10 better within ∼2″, and improve even further at larger separations. Right: the flux sensitivities on the left are translated to 5σ detection limits in terms of planet mass. For a nominal system age of 700 Myr, two models of atmosphere evolution are considered—BEX-HELIOS (solid line; E. F. Linder et al. 2019) and Ames-COND (dashed line; I. Baraffe et al. 2003)—with similar results from both. A younger age (e.g., 450 Myr; J. Yoon et al. 2010) would correspond to planet masses lower by ∼30% (dotted line), while the upper limit from J. D. Monnier et al. (2012; 850 Myr) would result in slightly higher masses (dotted–dashed line).
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 left) contrast curves (5σ) for Vega, Fomalhaut (M. Ygouf et al. 2024), and HR 8799 (G. Bryden et al. 2024). The differences are consistent with the brightness of the host star and the observation parameters as discussed in the text. (Top right) limiting magnitudes toward each star. (Bottom left) limiting mass sensitivity curves as a function of angular separation for the three stars using BEX models (E. F. Linder et al. 2019). A selection of directly imaged planets with model masses < 13 M J from the NASA Exoplanet Archive are plotted as black circles; the four HR 8799 planets are highlighted as red squares. For HR 8799 the region interior to HR 8799 b (1.″7, 80 au) is omitted to recognize the four high-mass planets found interior to this separation. The bump in the Vega curve at 175 au shows the edge of the coronagraphic mask. (Bottom right) same as for the bottom left panel but plotted as a function of physical separation. The mass curves and the points for HR 8799 are corrected for projection effects—5° inclination for Vega (J. D. Monnier et al. 2012), 67° for Fomalhaut (A. Gáspár et al. 2023), and 26° for HR 8799 (B. Matthews et al. 2014).
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) simple RDI subtraction of the F444W images of Vega and Deneb to search for disk emission. Arc-shaped annuli laying between the major Vega diffraction spikes were examined for disk emission as a function of distance from Vega. The dotted box denotes a region used as a background region to measure emission away from the annuli. (Bottom) the blue and orange lines denote emission within the partial annuli as a function of separation from Vega minus the background level in a vertical band at the right side of the image. The feature at ∼10″ is an artifact visible in the image and in the background trace and is due to the edge of the coronagraphic optical mount.