adsabs/AstroCLIMB huggingface dataset:
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Point-source completeness based on artificial star tests (see Section 3.2) from the central 20′ of the NE field. Blue and red points represent the g- and i-band completeness, respectively. The overlaid lines are the fits of Equation (1) to the completeness values. The lower two panels compare the injected and measured magnitudes of artificial stars; there is no magnitude bias evident. The NE field is the deepest in both g and i bands of all our seven fields; the 50% and 90% completeness results from all fields are given in Table 3 along with the 10σ point-source depths.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: RGB star selection. Left: objects in an elliptical annulus between semimajor axes of 14 < a < 20′ of the center of NGC 2403, at a position angle of 124° (Barker et al. 2012). Middle: between 2′ and 4′ from the center of DDO 44. Left: within 20″ of MADCASH-1. The black region in each panel outlines the RGB star selection. Isochrones in each panel are from A. Bressan et al. (2012), for metallicities of [M/H] = −2.0, −1.5, −1.0, and −0.5 and age 10 Gyr at a distance modulus of m − M  =  27.39 (J. L. Carlin et al. 2016).
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: An illustration of our method for star/galaxy separation. The ratio of point-spread-function (PSF) and cmodel fluxes is plotted against the i-band PSF magnitude. Point-like objects (i.e., “stars”) should have f PSF/f cmodel ∼ 1, while extended objects have more flux in the galaxy model measurement, scattering them to f PSF/f cmodel < 1. Objects are classified as likely stars (highlighted in black in the diagram) if they are within 3% (accounting for their measurement errors) of unity in this figure.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Luminosity (M  V ) vs. half-light radius (r h) for known satellites of MC-mass hosts in the Local Volume. Open gray symbols show the Milky Way and M31 satellites, with open black squares and triangles depicting (candidate) LMC and M33 satellites, respectively. Solid black symbols represent dwarf satellites of nearby (1 < D < 4 Mpc) MC-mass host galaxies for NGC 2403 (MADCASH 1, DDO 44); NGC 4214 (MADCASH 2); NGC 3109 (Antlia, Antlia B); NGC 55 (NGC 55-dw1, ESO 294-G010); and NGC 4449 (NGC 4449B, DDO 125). Symbols that are outlined are dwarfs that are known to be tidally disrupting.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Example diagnostic plot of a detection of (a portion of) DDO 44. The upper left panel shows a CMD, with candidate RGB stars highlighted in red and all point sources within a 1′ radius shown in blue. The upper right panel displays the spatial distribution of sources, using the same color-coding. In the middle left plot, we show a radial surface density plot (note that the center may not be properly located on the center of the overdensity, as we have not refined the measurements at this point). The middle right panel shows a color image of the region, and the lower right panel is the same image with RGB stars overlaid. In the lower left plot, we show an “LF” of candidate RGB stars; if a dwarf stellar population is present, one would expect the candidate dwarf (in red) to have a different LF than the neighboring field stars (shown in gray), as it does here for DDO 44.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Diagnostic plots for the dwarfs from the top row of Figure 7, with surface brightnesses of ∼29.0 mag arcsec−2, and (from left to right) M  V  ≈ −6.5, −7.5, and −8.5.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Example diagnostic plot showing the detection of MADCASH-1, the previously known ultrafaint dwarf near NGC 2403. Panels are as in Figure 11. The metal-poor RGB of MADCASH-1 is discernible in the CMD (upper left panel), but one can see in the images that the system is semiresolved, and thus, only a small number of stars are detected in the region of the semiresolved “fluff” around this ultrafaint dwarf.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Example diagnostic plot showing a candidate detection that is highly unlikely to be a dwarf galaxy associated with NGC 2403. Note that the LF of objects detected within the RGB box does not resemble a typical LF for stars in a dwarf galaxy but rather looks as if it was drawn from the (unresolved) background galaxy population.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Diagnostic plots for the dwarfs from the middle row of Figure 7, with surface brightnesses of ∼27.5 mag arcsec−2, and (from left to right) M  V  ≈ − 6.5, −7.5, and −8.5. Note that the middle panel in Figure 7 was replaced with an image of MADCASH-1; the middle set of diagnostic plots above are for a synthetic dwarf with M  V  ≈ −7.5 and μ ≈ 27.5 mag arcsec−2.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Diagnostic plots for the dwarfs from the top row of Figure 7, with surface brightnesses of ∼26.0 mag arcsec−2, and (from left to right) M  V  ≈ −6.5, −7.5, and −8.5.
Paper: A Census of Dwarf Galaxy Satellites around LMC-mass Galaxy NGC 2403 
Authors: Jeffrey L. Carlin, David J. Sand, Burçin Mutlu-Pakdil, Denija Crnojević, Amandine Doliva-Dolinsky, Christopher T. Garling, Annika H. G. Peter, Jean P. Brodie, Duncan A. Forbes, Jonathan R. Hargis, Aaron J. Romanowsky, Kristine Spekkens, Jay Strader, Beth Willman
Figure caption: Example diagnostic plot. This particular plot shows a portion of the DDO 44 stream, detected a few arcminutes from the center of DDO 44. The RGB is clearly visible in the upper left panel (CMD).
Paper: Exploring Pulsar Timing Precision: A Comparative Study of Polarization Calibration Methods for NANOGrav Data from the Green Bank Telescope
Authors: Lankeswar Dey, Maura A. McLaughlin, Haley M. Wahl, Paul B. Demorest, Zaven Arzoumanian, Harsha Blumer, Paul R. Brook, Sarah Burke-Spolaor, H. Thankful Cromartie, Megan E. DeCesar, Timothy Dolch, Justin A. Ellis, Robert D. Ferdman, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Nate Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Ross J. Jennings, Megan L. Jones, Michael T. Lam, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Cherry Ng, David J. Nice, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Renée Spiewak, Ingrid H. Stairs, Kevin Stovall, Joseph K. Swiggum
Figure caption: Example polarimetric response solutions used for different polarization calibration methods to calibrate the observed pulsar profiles. In all the panels G, γ, and ϕ represent the absolute gain, differential gain, and differential phase of the observing system, respectively. The absolute gain G is specified in units of the square root of the reference flux density (c 0). Panel (a): IFA PR solution obtained from the reference noise diode observation for PSR J1744−1134 on MJD 56614. Panels (b), (c), and (d): MEM PR solutions at 800 MHz calculated from long-track (∼3.5 hr) observations of PSR B1929+10 on MJDs 56244, 56419, and 56608, respectively. Here, θ 1 represents the orientation of receptor 1 with respect to receptor 0, and ϵ  k  represents the ellipticity angles of the two receptors (denoted by black and red points; see W. van Straten 2004, for details). Panel (e): MEM PR solution for Rcvr1_2, where δ  θ,χ  and σ  χ  represent the quantities as defined by Equation (17) of M. C. Britton (2000). Panel (f): METM-generated PR correction, calculated using a PSR B1937+21 observation on MJD 56614, to the MEM-generated PR on MJD 56608. Here, θ  k  and ϵ  k  represent the orientations and ellipticities of the two receptors (black and red points), respectively. Note that the absolute gain is not calculated for the METM-generated PR correction, as we used the total invariant interval to normalize the Stokes parameters. See Section 3.1 for more details.
Paper: Exploring Pulsar Timing Precision: A Comparative Study of Polarization Calibration Methods for NANOGrav Data from the Green Bank Telescope
Authors: Lankeswar Dey, Maura A. McLaughlin, Haley M. Wahl, Paul B. Demorest, Zaven Arzoumanian, Harsha Blumer, Paul R. Brook, Sarah Burke-Spolaor, H. Thankful Cromartie, Megan E. DeCesar, Timothy Dolch, Justin A. Ellis, Robert D. Ferdman, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Nate Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Ross J. Jennings, Megan L. Jones, Michael T. Lam, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Cherry Ng, David J. Nice, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Renée Spiewak, Ingrid H. Stairs, Kevin Stovall, Joseph K. Swiggum
Figure caption: Uncalibrated and calibrated (using different methods) polarization profiles of PSR J1909−3744 in the Rcvr1_2 band (1500 MHz). The calibration methods used to obtain the profiles are denoted in the plot titles. In each panel, the black, red, and blue lines indicate the total intensity (I), linear polarization (L), and circular polarization (V), respectively. Using the IAU's circular polarization sign convention, right-handed circular polarization is positive and left-handed circular polarization is negative.
Paper: Exploring Pulsar Timing Precision: A Comparative Study of Polarization Calibration Methods for NANOGrav Data from the Green Bank Telescope
Authors: Lankeswar Dey, Maura A. McLaughlin, Haley M. Wahl, Paul B. Demorest, Zaven Arzoumanian, Harsha Blumer, Paul R. Brook, Sarah Burke-Spolaor, H. Thankful Cromartie, Megan E. DeCesar, Timothy Dolch, Justin A. Ellis, Robert D. Ferdman, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Nate Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Ross J. Jennings, Megan L. Jones, Michael T. Lam, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Cherry Ng, David J. Nice, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Renée Spiewak, Ingrid H. Stairs, Kevin Stovall, Joseph K. Swiggum
Figure caption: Intrinsic Stokes parameters of the noise diode reference signal for Rcvr_800, plotted as a function of observing frequency for three distinct epochs: MJDs 56244, 56419, and 56608. The modeled values of Stokes Q, U, and V are expressed as percentages of the total intensity of the reference source.
Paper: Exploring Pulsar Timing Precision: A Comparative Study of Polarization Calibration Methods for NANOGrav Data from the Green Bank Telescope
Authors: Lankeswar Dey, Maura A. McLaughlin, Haley M. Wahl, Paul B. Demorest, Zaven Arzoumanian, Harsha Blumer, Paul R. Brook, Sarah Burke-Spolaor, H. Thankful Cromartie, Megan E. DeCesar, Timothy Dolch, Justin A. Ellis, Robert D. Ferdman, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Nate Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Ross J. Jennings, Megan L. Jones, Michael T. Lam, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Cherry Ng, David J. Nice, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Renée Spiewak, Ingrid H. Stairs, Kevin Stovall, Joseph K. Swiggum
Figure caption: Polarization profiles for PSR J1909−3744 observed with the GUPPI 800 MHz receiver system at GBT. Both uncalibrated profiles and profiles obtained by different calibration methods are shown.
Paper: Exploring Pulsar Timing Precision: A Comparative Study of Polarization Calibration Methods for NANOGrav Data from the Green Bank Telescope
Authors: Lankeswar Dey, Maura A. McLaughlin, Haley M. Wahl, Paul B. Demorest, Zaven Arzoumanian, Harsha Blumer, Paul R. Brook, Sarah Burke-Spolaor, H. Thankful Cromartie, Megan E. DeCesar, Timothy Dolch, Justin A. Ellis, Robert D. Ferdman, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Nate Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Ross J. Jennings, Megan L. Jones, Michael T. Lam, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Cherry Ng, David J. Nice, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Renée Spiewak, Ingrid H. Stairs, Kevin Stovall, Joseph K. Swiggum
Figure caption: Uncalibrated and different calibrated profiles for J1643−1224 observed with the Rcvr_800 (800 MHz) and Rcvr1_2 (1500 MHz) receivers and GUPPI backend system at the GBT.
Paper: Exploring Pulsar Timing Precision: A Comparative Study of Polarization Calibration Methods for NANOGrav Data from the Green Bank Telescope
Authors: Lankeswar Dey, Maura A. McLaughlin, Haley M. Wahl, Paul B. Demorest, Zaven Arzoumanian, Harsha Blumer, Paul R. Brook, Sarah Burke-Spolaor, H. Thankful Cromartie, Megan E. DeCesar, Timothy Dolch, Justin A. Ellis, Robert D. Ferdman, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Nate Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Ross J. Jennings, Megan L. Jones, Michael T. Lam, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Cherry Ng, David J. Nice, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Renée Spiewak, Ingrid H. Stairs, Kevin Stovall, Joseph K. Swiggum
Figure caption: Uncalibrated and different calibrated profiles for J1744−1134 observed with the Rcvr_800 (800 MHz) and Rcvr1_2 (1500 MHz) receivers and GUPPI backend system at the GBT.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. III. The Contribution of Planetesimals beyond Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the accreted planetesimal mass as a percentage of the initially available mass in the region of 8–12 au. Each panel shows the results for 1 and 100 km ice, rock, and mixed planetesimals. From top to bottom, the panels correspond to three different values of the mass of the outer planet.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. III. The Contribution of Planetesimals beyond Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the final eccentricity of the planetesimal (red dots) in terms of its initial semimajor axis. The black dots show the planetesimal’s initial eccentricity. The top panel represents the results for the mass of the exterior planet equal to 0.1 Saturn and the lower panel corresponds to the full Saturn mass.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. III. The Contribution of Planetesimals beyond Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Top: graphs of the time variations of the density of the envelope at different distances from the center of the protogiant planet based on the models described by M. Lozovsky et al. (2017). Shown are gas densities of 10−7 g cm−3 (blue line), 10−5 g cm−3 (green line), and 10−3 g cm−3 (red line). The radius of the core is shown by the black line. Bottom: graph of the time variation of the total mass of the planet. Note the runaway gas accretion and collapse of the envelope at 1.7 Myr.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. III. The Contribution of Planetesimals beyond Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the mass of the ejected planetesimals as a percentage of the initially available mass at 8–12 au. The color coding is similar to Figure 3, corresponding to 1 and 100 km planetesimals of rock, ice, and a mixture of ice and rock. From top to bottom, each panel corresponds to a different value of the mass of the outer planet.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. III. The Contribution of Planetesimals beyond Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graph of the percentage of all captured planetesimals for different values of the mass of the outer planet, in terms of their initial semimajor axes.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. III. The Contribution of Planetesimals beyond Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the accreted planetesimal mass as a percentage of the initially available mass in the region of 8–12 au for 100 km rock and 1 km ice. Each panel shows the results for three different values of the mass of the outer planet.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. III. The Contribution of Planetesimals beyond Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the planetesimal mass accreted by the outer planet as a percentage of the initial mass of the planetesimals in the region of 8–12 au. The color coding is similar to Figure 3.
Paper: Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Infrared spectra of amorphous and crystalline HNCO, isocyanic acid, each ice being made and its spectrum recorded at the temperature indicated. Each ice’s thickness was about 0.12 μm. The upper spectrum has been offset vertically by 0.15 for clarity.
Paper: Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Examples of Beer’s Law plots used to determine IR absorption coefficients and band strengths. These are for amorphous and crystalline HNCO, with the ices made and the spectra recorded at 10 and 120 K, respectively.
Paper: Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Molar refractions of four amorphous ices as a function of the number of methylene (-CH2-) groups of the molecule. From the lower left to the upper right in the graph, the points are for formic acid, methyl formate, methyl acetate, and methyl propionate. Values of Rm  are from R. L. Hudson et al. (2020a).
Paper: Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Beer’s Law plots used to determine IR band strengths for H2CO in H2O + H2CO ices with the ices made and the spectra recorded at 10 K. Open (white) circles are for six H2O + H2CO (28:1) ices and closed (black, filled) circles are for four H2O + H2CO (8.5:1) ices.
Paper: Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Molar refractions of four amorphous aldehyde ices as a function of the number of methylene (-CH2-) groups of the molecule. From the lower left to the upper right in the graph, the points are for formaldehyde, acetaldehyde, propionaldehyde, and butyraldehyde (R. L. Hudson et al. 2020a).
Paper: Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Three infrared spectra of solid isocyanic acid, HNCO, scaled to the same height. (a) Transmission mode, scanned from M. S. Lowenthal et al. (2002), (b) transmission mode, this work, (c) reflection mode, scanned from S. Raunier et al. (2003). Each ice was made and the spectrum recorded at the temperature indicated.
Paper: Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Infrared spectrum of amorphous H2CO, formaldehyde. The ice was made and the spectrum recorded at 10 K. This ice’s thickness was about 1.01 μm.
Paper: Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Near-IR optical constants of amorphous H2CO, formaldehyde. Values of n and k were calculated from the IR spectra of eight ices and then averaged to give the results shown here. Each ice was made and its spectrum was recorded at 10 K. The ices used to calculate these optical constants varied in thickness from about 0.25–2.01 μm.
Paper: Infrared Band Strengths and Other Properties of Three Interstellar Compounds—Amorphous Isocyanic Acid, Formaldehyde, and Formic Acid
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Perry A. Gerakines
Figure caption: Mid-IR optical constants of amorphous H2CO, formaldehyde. Values of n and k were calculated from the IR spectra of eight ices and then averaged to give the results shown here. Each ice was made and its spectrum was recorded at 10 K. The ices used to calculate these optical constants varied in thickness from about 0.25 to 2.01 μm.