adsabs/AstroCLIMB huggingface dataset:
Paper: Optical Variability of Eight FRII-type Quasars with 13 yr Photometric Light Curves
Authors: Agnieszka Kuźmicz, Arti Goyal, Stanisław Zola, Marek Jamrozy, Marek Dróżdż, Waldemar Ogłoza, Michał Siwak, Daniel E. Reichart, Vladimir V. Kouprianov, Daniel B. Caton
Figure caption: Anticorrelation between the projected linear size of radio structures (D) and PSD slope (β).
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Scale model of the core of the interstellar grain. The thick lines show three types of allowed CR tracks through the grain. Track types along the other two symmetry axis are also possible but are not shown for clarity.
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Example energy spectra for oxygen CR nuclei at a different A  V  value for each curve, with N H/A  V  = 2.20 × 1021 cm−2.
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Energy spectra for selected cosmic-ray components at N H = 8.80 × 1022 cm−2, corresponding to A  V  = 40 mag.
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Energy-loss function L gas for CR species traversing interstellar matter; E lost includes also losses due to ISM atoms other than H.
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Heat capacities C for grain constituents.
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Left to right: cross sections of bare (a) and icy interstellar grain models with thin (b) and thick (c) icy mantles (see Figure 1 for bare grain). Different possible CR tracks are identified using the convention “g” (tracks pass only through the refractory nucleus of the grain), “i” (tracks pass only through ice), and “gi” (tracks pass through ice and the grain nucleus).
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Comparison of CR-induced whole-grain-heating frequency f  T  for T CR above 27 K and 70 K by different authors. References: K18/22: Paper IIa; HH93: Hasegawa & Herbst (1993); R+07: Roberts et al. (2007); LJO85: Leger et al. (1985); S+04: Shen et al. (2004).
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Energy E grain spectra for grains with core sizes 0.05, 0.1, and 0.2 μm hit by cosmic rays at A  V  1.5, 3.0, 6.0, 9.0, 20, 40, 80, and 160 mag, with N H/A  V  = 2.20 × 1021 cm−2.
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Temperature spectra for grains with core sizes 0.05, 0.1, and 0.2 μm hit by cosmic rays at A  V  1.5, 3.0, 6.0, 9.0, 20, 40, 80, and 160 mag, with N H/A  V  = 2.20 × 1021 cm−2.
Paper: Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. III. Mixed-composition Grains
Authors: Juris Kalvāns, Juris Roberts Kalnin
Figure caption: Energy-loss functions L grain for magnesium CR nuclei traversing different grain materials.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Light curves and the results of cross-correlation analysis for the season of 2015. The top panel shows the photometric light curve of NGC 5548 (instrument magnitude of V band) obtained from the Lijiang 2.4 m telescope during the spectroscopic monitoring periods, which is used to check the quality of the spectral calibration. The left panels (a)–(e) are the light curves of the AGN continuum at 5100 Å and the broad He II, He I, Hγ, and Hβ lines; the contamination of the host galaxy on this data has been eliminated by spectral decomposition. The right panels (aa)–(ea) correspond to the autocorrelation function (ACF) of the continuum and the cross-correlation function (CCF) between the broad-line light curves (b)–(e) and the continuum variation (a); the histogram in blue is the cross-correlation centroid distribution (CCCD). We note the variability amplitude F var (%) in panels (b)–(e), and the maximum cross-correlation coefficient r max in CCF panels (ba)–(ea). The measured time lag is marked by the vertical dotted lines in panels (ba)–(ea). The units of F 5100 and the emission lines are erg s−1 cm−2 Å−1 and erg s−1 cm−2, respectively.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Multicomponent fitting and decomposition of mean spectrum calculated from the season of 2015. Panel (a) shows the details of the spectral fitting and decomposition, where the mean spectrum is shown in lime, and the fitting components are noted in the legend. Panel (b) shows the fitting residuals in percentage. Panel (c) shows the net broad Hγ, He II, Hβ, and He I lines, where the fitted broad-line profiles (models) are shown as red dashed lines, and the broad-line profiles obtained by subtracting other fitted components from the spectrum are shown as black lines.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Same as Figure 7, but for the season of 2021.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Same as Figure 6, but for the season of 2018; the top panel shows the photometric light curve of NGC 5548 (g-band) obtained from ASAS-SN during the spectroscopic monitoring periods.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Same as Figure 7, but for the season of 2020. Because the maximum cross-correlation coefficients between the light curves of broad He I (and Hγ) lines and the varying 5100 Å continuum are far less than 0.5, the relevant results are not displayed in this figure.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Same as Figure 4, but for the seasons of 2018, 2019, 2020, and 2021.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Mean and rms spectra of each season calculated from the processed spectra (see Section 2.2); the legend in panel (a) marks the seasons of 2015, 2018, 2019, 2020, and 2021. Just narrow emission lines (such as narrow Hγ, He II, Hβ, [O III], and He I) are subtracted by spectral fitting and decomposition (see Section 3.2) before calculation.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: We randomly select one spectrum per season from the calibrated ones (see Section 2.2) to showcase the spectral quality. The Julian date (and calendar date) and S/N at 5100 Å are noted in each panel.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Same as Figure 7, but for the season of 2019.
Paper: An Early Catalog of Planet-hosting Multiple-star Systems of Order Three and Higher
Authors: M. Cuntz, G. E. Luke, M. J. Millard, L. Boyle, S. D. Patel
Figure caption: Display of the planetary eccentricity as a function of the semimajor axis pertaining to confirmed planet-hosting triple-star systems. Planets of single and multiple planetary systems are depicted by blue and red data points, respectively. If the eccentricity is assumed to be zero (instead of measured), a triangle is used.
Paper: An Early Catalog of Planet-hosting Multiple-star Systems of Order Three and Higher
Authors: M. Cuntz, G. E. Luke, M. J. Millard, L. Boyle, S. D. Patel
Figure caption: Display of the planet’s mass as a function of the semimajor axis pertaining to confirmed planet-hosting triple-star systems. Planets of single and multiple planetary systems are depicted by blue and red data points, respectively. An arrow is used when only the planet’s minimum or maximum mass is known.
Paper: An Early Catalog of Planet-hosting Multiple-star Systems of Order Three and Higher
Authors: M. Cuntz, G. E. Luke, M. J. Millard, L. Boyle, S. D. Patel
Figure caption: Number count of stellar spectral types for primary, secondary, and tertiary stars pertaining to planet-hosting triple-star systems. The left bars refer to confirmed systems, whereas the right bars refer to unconfirmed systems. There are also a small number of objects of spectral type L and T not depicted here.
Paper: An Early Catalog of Planet-hosting Multiple-star Systems of Order Three and Higher
Authors: M. Cuntz, G. E. Luke, M. J. Millard, L. Boyle, S. D. Patel
Figure caption: Display of the planet’s mass as a function of the host’s stellar mass pertaining to confirmed planet-hosting triple-star systems. Planets of single and multiple planetary systems are depicted by blue and red data points, respectively. An arrow is used when only the planet’s minimum or maximum mass is known.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Variations of the optical luminosity (panel (a)) and the BLR radius (panel (b)) for NGC 5548 measured between 1988 and 2021, and the result of cross-correlation analysis (panel (ba)). Different symbols with different colors are used in the left panels to distinguish between the different campaigns. In panel (ba), the red solid curve is the CCF between the BLR radius and the optical luminosity measured between 1988 and 2021 (﹩{r}_{\max }=0.66﹩), and the blue solid histogram is the CCCD; the measured time lag of ﹩{3.5}_{-1.8}^{+2.0}﹩ yr is marked by the vertical dotted line in black. A subset of the BLR radius and the optical luminosity measured after 1997 (marked as a vertical dashed line in panels (a) and (b)) is selected to recalculate the time lag. The result is also shown in panel (ba), where the red dashed curve is the CCF between the BLR radius and the optical luminosity measured between 1997 and 2021 (﹩{r}_{\max }=0.87﹩), and the blue dashed histogram is the CCCD; the measured time lag of ﹩{4.6}_{-1.3}^{+1.7}﹩ yr is marked by the vertical dotted line in gray.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: The results of velocity-resolved RM analysis for the seasons of 2015, 2018, 2019, and 2021. For each season, panel (a) shows the rms spectrum of broad Hγ (left) or Hβ (right), and panel (b) shows the centroid time lags as a function of velocity in the line of sight. The vertical dotted lines are the edges of the velocity bins. The Hγ and Hβ VRLPs are plotted in the same coordinate ranges in the direction of the velocity axis. All maximum cross-correlation coefficients between the velocity-binned light curves and the varying AGN continuum at 5100 Å are larger than 0.5. Note that the broad-line velocity binning is below the instrumental resolution of ∼695 km s−1, and thus the measurements are not independent.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Relation between the optical luminosity at 5100 Å and the Hβ time lag from 23 RM campaigns for NGC 5548 (see the inserted legend). The black dotted–dashed line is the canonical R Hβ –L 5100 relation with a slope of 0.53 (Bentz et al. 2013), and the dotted lines are the intrinsic scatter (±0.13 dex) of this relation. The blue dotted–dashed line is the best fit for data of NGC 5548, which gives a slope of 0.57 with an intrinsic scatter of 0.26 dex; the fitted relation is recorded at the bottom of the figure. The average values of τ Hβ  and L 5100 over the 23 campaigns (green diamond) are consistent with the canonical R Hβ –L 5100 relation. The previous RM measurements are shown in symbols of circles, and our five-season RM measurements are shown as “⋆.” The different symbols with different colors are used to distinguish the different campaigns.
Paper: Optimal Defocus for Phase Diversity Wave Front Retrieval
Authors: F. J. Bailén, D. Orozco Suárez, J. Blanco Rodríguez, J. C. del Toro Iniesta
Figure caption: Top: full incident wave front (solid black) and retrieved wave fronts expanded up to the 32nd Zernike order for Δ = −0.5λ (red dashed–dotted), Δ = −1λ (blue dashed), Δ = −1.5λ (green dotted), and Δ = −2λ (magenta dotted). Bottom: residual of the wave front fitting for each case displayed in the top panel.
Paper: Optimal Defocus for Phase Diversity Wave Front Retrieval
Authors: F. J. Bailén, D. Orozco Suárez, J. Blanco Rodríguez, J. C. del Toro Iniesta
Figure caption: Performance of PD against Δ for the scene displayed in Figure 2. Top: rms error of the Zernike coefficients fitting for different values of J as a function of the defocus. Bottom: value of Δ that produces the best wave front fitting for each choice of J (blue) and its corresponding rms error (red).
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Relation between the broad-line widths and their time lags for NGC 5548; the colorful circles are the new measurements from this work, and the black circles are the previous measurements. The broad-line width can be characterized by either the FWHM or the line dispersion (σ line), and both can be measured from the mean or rms spectra. For each case, the dotted–dashed lines are the fit to the relation of ﹩\mathrm{log}\,(\mathrm{FWHM}\,\mathrm{or}\,{\sigma }_{\mathrm{line}})=a+b\,\mathrm{log}\,\tau ﹩, and the results of the best fit are recorded at the bottom of each panel. The dotted lines are the best fit with a forced virial slope of b = −0.5.
Paper: Optimal Defocus for Phase Diversity Wave Front Retrieval
Authors: F. J. Bailén, D. Orozco Suárez, J. Blanco Rodríguez, J. C. del Toro Iniesta
Figure caption: (a) Original MHD simulation. (b) Focused image obtained after degrading (a) with the wave front and adding noise. (c) Defocused image obtained as in (b) and by adding a defocus term with Δ = −1.5λ. (d) Restored image using the pair of images in panels (b) and (c) while setting J to 32.
Paper: Supermassive Black Hole and Broad-line Region in NGC 5548: Results from Five-season Reverberation Mapping
Authors: Kai-Xing Lu, Jin-Ming Bai, Jian-Min Wang, Chen Hu, Yan-Rong Li, Pu Du, Ming Xiao, Hai-Cheng Feng, Sha-Sha Li, Jian-Guo Wang, Zhi-Xiang Zhang, Ying-Ke Huang
Figure caption: Relation between the Hβ-based line dispersion (σ line) and optical luminosity of NGC 5548. The same symbols in Figures 13 and 14 are used to distinguish between the different campaigns. To guide the eye, a dotted line with a slope of −0.5 is plotted over the data from this work.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Output of the spatially resolved SED fit on Arp 220. The top row, from left to right, shows the RGB image (built combining three broadband filters), the stellar mass density map, and the SFRD maps inferred with the stellar continuum and with the Paβ emission-line flux. The bottom row shows the resulting Hα and Paβ surface density flux maps, as well as the A  V  inferred from the empirical Balmer-to-Paschen decrement, and the stellar continuum. The cross is centered on the brightest F110W pixel. The physical scale is indicated on the A  V  continuum panel (bottom right).
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for IRASF10038-3338. See Figure 19 for more details.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for IRAS13120-5453. See Figure 19 for more details.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for IRAS23436+5257. See Figure 19 for more details.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for IRAS08355-4944. See Figure 19 for more details.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for IRAS03582+6012. See Figure 19 for more details.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for IRAS12116-5615. See Figure 19 for more details.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for IRAS18090+0130. See Figure 19 for more details.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for ESO550-IG025. See Figure 19 for more details.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for IRASF16399-0937. See Figure 19 for more details.
Paper: High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines
Authors: Clara Giménez-Arteaga, Gabriel B. Brammer, Danilo Marchesini, Luis Colina, Varun Bajaj, Malte Brinch, Daniela Calzetti, Daniel Lange-Vagle, Eric J. Murphy, Michele Perna, Javier Piqueras-López, Gregory F. Snyder
Figure caption: Maps of the physical properties inferred with our SED fitting code for IRASF16164-0746. See Figure 19 for more details.