adsabs/AstroCLIMB huggingface dataset:
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Single scattering albedo w 0, optical depth per layer OPD, and asymmetry parameter g 0 for the condensation cloud model computed with Virga, as well as the micrometeoroid dust model. The combination of the two is the optical depth–weighted average for the scattering parameters or the sum of the optical depths themselves. This particular simulation uses grid temperature T grid = 800 K, surface gravity g = 316 m s−1, vertical eddy diffusion coefficient K  zz  = 105 cm2 s−1, sedimentation efficiency f sed = 10, dust power-law index α = −3.5, and dust power-law coefficient ﹩\mathrm{log}{N}_{0}=14﹩.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Discrete approximation to posterior probability distributions for disequilibrium atmospheric model parameters of 51 Eridani b. Parameter-pair covariance surfaces use a black-hot color map, while single-parameter posteriors are scaled such that the y-axis begins at likelihood ﹩{ \mathcal L }=0﹩. The 16th, 50th, and 84th percentile values are shown in red, with corresponding values printed on the top of the panel.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Total infalling dust mass as a function of dust power-law model parameters.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Optical contribution of major gaseous absorbers in the disequilibrium (solid) and equilibrium (dotted) chemistry models. Curves correspond to pressures where the approximate cumulative optical depth per species is of order unity. The high-altitude CO in the disequilibrium model is evidently responsible for additional absorption in the range of 4–5 μm. This feature is generally visible in all of the disequilibrium models, but exactly how much varies with atmospheric parameters. This specific realization uses grid temperature T grid = 800 K, surface gravity g = 316 m s−1, sedimentation efficiency f sed = 10, and vertical eddy diffusion coefficient ﹩\mathrm{log}\tfrac{K\mathrm{zz}}{{\mathrm{cm}}^{2}/{\rm{s}}}=5﹩.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Molecular volume mixing ratios comparing the equilibrium and disequilibrium abundances as a function of pressure altitude. The significant presence of CO in the disequilibrium model is highlighted with a thick curve. Molecules are roughly grouped into color families, and labels are constrained to the same y-coordinate in both panels. Additional species noticeably affected by the disequilibrium chemistry include N2, NH3, CO2, and HCN.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Best-fit model spectra from each unique model class. Although the equilibrium chemistry models are optimal from the perspective of ﹩{\chi }_{\nu }^{2}﹩, they struggle to fit the M-band photometric point. This single point does not have a large influence on the final ﹩{\chi }_{\nu }^{2}﹩ compared to the spectroscopic bands in JHK, which have a much greater information content. The dusty models generally do not perform better than the dust-free models.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Scattering parameters as a function of wavelength and particle size. As in Figure 9, blue corresponds to nanometer-sized particles, while red corresponds to millimeter-sized particles. One can see that the millimeter-sized particles strongly forward scatter with a scattering asymmetry parameter of g ≈ 0.8, while the nanometer-sized particles scatter nearly isotropically with g ≈ 0. In the right panel, the horizontal dashed lines correspond to the geometric cross section for an equivalently sized sphere. For particles of size with the same order of magnitude as the wavelength, the Mie and geometric cross sections are very similar, but the cross section drops off dramatically for the nanometer-sized grains, especially for longer wavelengths. This fact alongside the effect of modifying the dust power-law index α allows the dust to modify the reddening of the spectra demonstrated in Figure 4.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Equilibrium chemistry and dusty atmospheric model posterior parameter distribution triangle plot.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Dust transport values as a function of pressure altitude and particle radius for a particular atmospheric realization with grid temperature T grid = 800 K, surface gravity g = 316 m s−1, dust power-law index α = −3.5, and dust power-law coefficient ﹩\mathrm{log}{N}_{0}=12﹩. Colored curves correspond to particles between radii r 1 = 1 nm and r 2 = 1 mm, with blue being the smallest particles and red the largest with logarithmic spacing between different lines.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Index of refraction for silicates from different sources. The black vertical lines indicate the range of wavelengths important to this study.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Equilibrium chemistry and dust-free atmospheric model posterior parameter distribution triangle plot.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Disequilibrium chemistry and dust-free atmospheric model posterior parameter distribution triangle plot.
Paper: The Infrared Colors of 51 Eridani b: Micrometeoroid Dust or Chemical Disequilibrium?
Authors: Alexander Madurowicz, Sagnick Mukherjee, Natasha Batalha, Bruce Macintosh, Mark Marley, Theodora Karalidi
Figure caption: Atmospheric parameters as a function of pressure altitude.
Paper: Comprehensive Study of the Chemical Composition and Spatial Outgassing Behavior of Hyperactive Comet 46P/Wirtanen Using Near-IR Spectroscopy during its Historic 2018 Apparition
Authors: Younas Khan, Erika L. Gibb, Nathan X. Roth, Michael A. DiSanti, Neil Dello Russo, Boncho P. Bonev, Chemeda T. Ejeta, Mohammad Saki, Ronald J. Vervack, Adam J. McKay, Hideyo Kawakita, Michael R. Combi, Danna Qasim, Yinsi Shou
Figure caption: Production rates of H2O (blue), HCN (green), CH3OH (black), and C2H6 (red) in 46P during its 2018 apparition. The December dates correspond to 2018, whereas the January and February dates correspond to 2019. Volatiles with only upper limits are not shown. The uncertainties in the production rates are shown. The heliocentric distances are shown at the top of the figure. The vertical dashed black and dotted red lines represent the dates of the perihelion and the closest approach to Earth, respectively. The values corresponding to UT 2018 December 18 and 21 and 2019 January 11–13 and February 4 are taken from Roth et al. (2021a), Khan et al. (2021), McKay et al. (2021), and Saki (2021), respectively.
Paper: Comprehensive Study of the Chemical Composition and Spatial Outgassing Behavior of Hyperactive Comet 46P/Wirtanen Using Near-IR Spectroscopy during its Historic 2018 Apparition
Authors: Younas Khan, Erika L. Gibb, Nathan X. Roth, Michael A. DiSanti, Neil Dello Russo, Boncho P. Bonev, Chemeda T. Ejeta, Mohammad Saki, Ronald J. Vervack, Adam J. McKay, Hideyo Kawakita, Michael R. Combi, Danna Qasim, Yinsi Shou
Figure caption: Emission spatial profiles of the primary volatiles and dust in 46P on UT 2018 December 6 ((A) and (B)), 14 ((C) and (D)), and 16 ((E), (F), and (G)). The profiles are color-coded, and comeasured profiles are overplotted on top of one another, after normalizing them to the profile with the highest intensity. The orientation of the slit on a given observing date along the Sun–comet line is indicated by the compass directions in panels (A), (C), and (E). The Sun–comet–Earth angle (phase angle, β) for each date is also shown in panels (B), (D), and (F). The UT intervals associated with the profiles are shown in each panel. The color-coded envelopes at the bottom of each panel represent the ±1σ uncertainties in the spatial profiles.
Paper: Comprehensive Study of the Chemical Composition and Spatial Outgassing Behavior of Hyperactive Comet 46P/Wirtanen Using Near-IR Spectroscopy during its Historic 2018 Apparition
Authors: Younas Khan, Erika L. Gibb, Nathan X. Roth, Michael A. DiSanti, Neil Dello Russo, Boncho P. Bonev, Chemeda T. Ejeta, Mohammad Saki, Ronald J. Vervack, Adam J. McKay, Hideyo Kawakita, Michael R. Combi, Danna Qasim, Yinsi Shou
Figure caption: Spatial profiles of the primary volatiles in 46P on 2018 December 19. (A)–(B) Comeasured CH3OH and C2H6, along with the comeasured dust profile, using PAs of 113° and 23°, respectively. (C) H2O and HCN overplotted on one another, along with the comeasured dust, using a PA of 113°. The Sun–comet–Earth angle (phase angle, β) is also shown in (C). The UT intervals that are associated with the profiles are shown in each panel. The color-coded envelopes at the bottom of each panel represent the ±1σ uncertainties in the spatial profiles.
Paper: Comprehensive Study of the Chemical Composition and Spatial Outgassing Behavior of Hyperactive Comet 46P/Wirtanen Using Near-IR Spectroscopy during its Historic 2018 Apparition
Authors: Younas Khan, Erika L. Gibb, Nathan X. Roth, Michael A. DiSanti, Neil Dello Russo, Boncho P. Bonev, Chemeda T. Ejeta, Mohammad Saki, Ronald J. Vervack, Adam J. McKay, Hideyo Kawakita, Michael R. Combi, Danna Qasim, Yinsi Shou
Figure caption: Mixing ratios with respect to H2O of the primary volatiles CH3OH and C2H6 (A), NH3 and H2CO (B), and HCN and C2H2 (C) in 46P during its 2018 apparition. The species are color-coded and the uncertainties in the mixing ratios are shown as the error bars. The 3σ upper limits of the mixing ratios are represented by the downward arrows. The heliocentric distances are shown at the top of each panel. The values corresponding to UT 2018 December 18 and 21 and 2019 January 11, 12, and 13 and February 4 and 5 are taken from Roth et al. (2021a), Khan et al. (2021), McKay et al. (2021), and Saki (2021), respectively. The vertical dashed black line represents the perihelion date, while the dotted red line shows the date of the closest approach to Earth.
Paper: Comprehensive Study of the Chemical Composition and Spatial Outgassing Behavior of Hyperactive Comet 46P/Wirtanen Using Near-IR Spectroscopy during its Historic 2018 Apparition
Authors: Younas Khan, Erika L. Gibb, Nathan X. Roth, Michael A. DiSanti, Neil Dello Russo, Boncho P. Bonev, Chemeda T. Ejeta, Mohammad Saki, Ronald J. Vervack, Adam J. McKay, Hideyo Kawakita, Michael R. Combi, Danna Qasim, Yinsi Shou
Figure caption: The production rates of H2O (blue), C2H2 (purple), and NH3 (brown) in 46P during 2018 December. The error bars show the uncertainties in the production rates. The heliocentric distances corresponding to all dates are shown at the top of the figure. The vertical dashed black line and the dotted red line represent the perihelion date and date of the closest approach to Earth, respectively. The values corresponding to UT 2018 December 21 are taken from Khan et al. (2021).
Paper: Comprehensive Study of the Chemical Composition and Spatial Outgassing Behavior of Hyperactive Comet 46P/Wirtanen Using Near-IR Spectroscopy during its Historic 2018 Apparition
Authors: Younas Khan, Erika L. Gibb, Nathan X. Roth, Michael A. DiSanti, Neil Dello Russo, Boncho P. Bonev, Chemeda T. Ejeta, Mohammad Saki, Ronald J. Vervack, Adam J. McKay, Hideyo Kawakita, Michael R. Combi, Danna Qasim, Yinsi Shou
Figure caption: Mixing ratios of the primary volatiles in 46P (black triangles) compared with the values in the comet population (open green triangles). The weighted means of the mixing ratios in 46P are represented by the blue circles, whereas the red diamonds represent the mean mixing ratios in the comet population sampled in the near-IR. The most significant 3σ upper limits in 46P are represented by the downward arrows. For the comets that are shown in this figure, see Table 3 in Dello Russo et al. (2016) and the notes to Table 3 in this work.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Left: reproduction of the Hα line emission image of NGC 5597 (Garcia-Barreto et al. 1996) in contours superposed on the H I 21 cm moment 0 in gray scale. The Hα image is not calibrated in flux density scale; therefore, the contours are proportional to the noise in arbitrary units from 3.5σ to 17σ. The most intense central emission of the hot gas, seen in Hα, is devoid of cold gas H I 21 cm emission. At least two Hα sources are offset by a few arcseconds to the N of the H I 21 cm sources. Right: our new 20 cm radio continuum emission image in contours superposed on the optical red (I-filter 8040 Å) image (Garcia-Barreto et al. 1996). The restoring beam size of the 20 cm continuum image at FWHM is ∼6.″11  ×  3.″7 (P.A. ∼ −8°). The contours are at 3σ, 4σ, 5σ, 6σ, 8σ, 10σ, 14σ, 18σ, 22σ, 26σ, 30σ, 40σ, 45σ, and 53σ, where 1σ ∼ 167.4 μJy beam−1. The strongest 20 cm radio continuum emission arises from an unresolved source coincident with the position of the optical nucleus with an inner elongated structure at P.A. ∼ 25° E of N. The peaks of the 20 cm continuum sources are labeled a–h as listed in Table 2.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Left panel: H I 21 cm spectrum of NGC 5597 obtained from VLA B-configuration observations. The heliocentric systemic velocity, fitted by the task GAL in AIPS, is V(sys)helio = 2698 km s−1, with ΔV 50% ∼ 211.40 and ΔV 20% ∼ 239.25 km s−1. The flux density scale is very difficult to compare to previous Parkes (64 m) and Green Bank (91 m) single-dish spectra because their beam included both disk galaxies NGC 5595 and NGC 5597 (Mathewson et al. 1992; Springob et al. 2005). The shape of the spectrum looks very similar to that obtained with Nançay; however, its beam at FWHM was ∼3.″6 E–W ﹩\times \,22^{\prime} ﹩ N–S (Paturel et al. 2003). Middle panel: H I 21 cm rotation curve of NGC 5597. Right panel: H I 21 cm angular velocity curve of NGC 5597.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Reproduction of optical red continuum image (broadband filter I 8040 Å), in gray scale and contours, of the disk galaxy NGC 5597 obtained with the OAN-SPM 2.1 m optical telescope in Mexico (Garcia-Barreto et al. 1996). The image has been convolved with a circular Gaussian beam of ∼1.″5 at FWHM. The flux density scale has not been calibrated; thus, the gray-scale stretch is from 5 → 37σ, where 1σ ∼ 45 is the noise in arbitrary units. Contours are at 5, 7, 11, 15, 20, 25, 30, 34, 40, 60, 80, 100, 200, 300, 400, 500, 750, 900 × 1σ.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Reproduction of the optical blue continuum image (glass plate 103aO) from the close pair of disk galaxies NGC 5597 to the SE and NGC 5595 to the NW, obtained with the OAN-SPM 2.1 m optical telescope in Mexico (Diaz-Hernández et al. 2009). The flux density scale has not been calibrated. The gray scale is from 2 → 27.8σ, where σ is the noise in arbitrary units.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Left: H I 21 cm VLA B-configuration integrated intensity over velocity, moment 0, image of NGC 5597 in contours superposed on gray scale. The contours are at 3, 35, 50, 70, 100, 125, 150, 175, 200, 250, 270 × 1σ ∼ 0.3 mJy beam−1 km s−1. The gray-scale stretch is from 3σ to 200σ. The synthesized beam at FWHM is shown in the lower left corner. The letter A indicates an isolated source as if it were in the center of a circular area devoid of H I emission. Right: optical I-filter image in contours (same as Figure 2) over H I (21 cm) moment 0 in gray scale, with gray-scale stretch from 2 to 17.5 mJy beam−1 km s−1.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Blueshifted H I 21 cm velocity field, moment 1, of NGC 5597 in contours superposed on the moment 0 gray-scale image. The gray scale ranges from 1 to 15 mJy beam−1 km s−1. Left: low blueshifted velocity contours from center to right at 2700, 2695, 2690, 2685, 2680, and 2675 km s−1. Right: high blueshifted velocity contours from center to right at 2670, 2665, 2660, 2655, 2650, 2645, 2640, 2635, 2630, 2625, and 2620 km s−1.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Redshifted H I 21 cm velocity field, moment 1, of NGC 5597 in contours superposed on the moment 0 gray-scale image. The gray scale in both panels ranges from 1 to 15 mJy beam−1 km s−1. Left: low redshifted velocity contours from center to left at 2700, 2705, 2710, 2715, 2720, 2725, and 2730 km s−1. Right: high redshifted velocity contours from center to left at 2735, 2740, 2745, 2750, 2755, and 2760 km s−1.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Innermost 20″ of NGC 5597. The filled triangle shows the kinematical center of the H I 21 cm emission, the four-pointed star shows the position of the photometric optical red I-filter image, and the filled circle shows the position of the photometric blue 103aO image. Spatial coordinates are listed in Table 2. Left: Hα continuum-free emission in contours superposed on the VLA B-configuration H I 21 cm moment 0 image in gray scale. The optical image is not calibrated in flux density scale, and the contour levels are at 7, 9, 11, 15, 20, 40, 80, 100, 300, 500, and 720 × 1σ, where 1σ = 10 in relative units. The gray scale ranges from 5.76 to 30 mJy beam−1 km s−1. The extended emission lies at P.A. ∼ 32° ± 14°. Right: our new VLA B-configuration 20 cm continuum emission in contours superposed on the H I 21 cm moment 0 image in gray scale. The contour levels are the same as in Figure 8(b). The NE extended 20 cm radio continuum is at P.A. ∼ 17° ± 7°. The gray scale ranges from 5 to 25 mJy beam−1 km s−1. Notice that the peak of the Hα emission (left panel) is slightly SW of the peak of the 20 cm radio continuum (right panel) that is associated with the optical nucleus. Qualitatively, both the 20 cm continuum and the Hα spatial emissions are similar. There is no cold gas atomic H I 21 cm emission (in gray scale) from the nucleus and the innermost circumnuclear region.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: The left panel shows the H I 21 cm velocity field of NGC 5595, moment 1, with blueshifted velocities in contours superposed on the moment 0 image in gray scale (the scale stretch is from 7.7 to 37 mJy beam−1 km s−1). Velocity contours from center to NE are at 2690, 2670, 2650, 2630, 2610, 2590, 2570, 2560, and 2550 km s−1. The right panel shows the redshifted velocity contours from center to SW at 2700, 2720, 2740, 2760, 2780, 2800, 2820, 2840, 2850, and 2855 km s−1. The velocity field indicates differential rotation, as expected from a disk galaxy. Notice that the uppermost NE contours show blueshifted velocities as if they were a smooth continuation from the blueshifted velocities from the inner disk, although the cold atomic H I 21 cm gas there has no optical counterpart. Similarly, the SW contours show redshifted velocities as if they were a smooth continuation from the redshifted velocities from the inner disk, although the cold atomic H I 21 cm gas there has no optical counterpart.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: The NGC 5595 VLA B-configuration H I 21 cm integrated intensity over velocity, moment 0, image in gray scale and contours. The contour levels are at 3, 6, 9, 12, 15, 20, 25, 30, 35, 40, and 47 × 1σ = 3.3 Jy beam−1 km s−1. Notice that there is no atomic hydrogen gas emission from the position of the kinematical center α(J2000.0) = 14h24m13.ˢ3, δ(J2000.0) = ﹩-16^\circ 43^{\prime} 21\buildrel{\prime\prime}\over{.} 6﹩. This position coincides with the optical continuum photometric center. The VLA B-configuration beam size, which is ∼7.″14  ×  4.″21 at FWHM, is shown in the lower left corner.
Paper: H I 21 cm Extended Structures to the Northeast and Southwest of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Left: H I 21 cm spectrum obtained from our VLA B-configuration observations of the disk galaxy NGC 5595. The heliocentric systemic velocity, fitted by the task GAL in AIPS, is V(sys)helio = 2702 km s−1, with ΔV 50% ∼ 317.5 and ΔV 20% ∼ 345 km s−1. The flux density scale of the spectrum is very difficult to compare to previous ones obtained with the Parkes (64 m) and Green Bank (91 m) radio telescopes because their beams included both disk galaxies, NGC 5595 and NGC 5597 (Mathewson et al. 1992; Springob et al. 2005). The shape of the spectrum looks very similar to that obtained with Nançay; however, its beam at FWHM was ∼3.″6 E–W ﹩\times \,22^{\prime} ﹩ N–S (Paturel et al. 2003). Middle: NGC 5595 H I 21 cm rotation curve. Right: NGC 5595 H I 21 cm angular velocity Ωgas.