adsabs/AstroCLIMB huggingface dataset:
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 MCG+12-02-001. 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 MCG-02-01-051. 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 NGC 2623. 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 NGC 6090. 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 NGC 2146. 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 NGC 5256. 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 NGC 5331. 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 VV340A. 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 NGC 6240. 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 NGC 6786. 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 NGC 6670. 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 NGC 7592. See Figure 19 for more details.
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: Year of discovery for the planet-hosting triple- and quadruple-star systems, as gauged by the year of publication pertaining to the planet(s); see main text for references. C-TSy and UC-TSy denote certain and uncertain planet-hosting triple-star systems, respectively, whereas C-QSy and UC-QSy denote certain and uncertain planet-hosting quadruple-star systems, respectively.
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 stellar hemisphere for R.A. between 0 and 12 hr. Stars of different magnitudes are depicted with the number of stars restricted to about 150. Additionally, we show the position of the various triple (triangles) and quadruple stellar systems (squares) with planets. See Table 4 for information on the color code for the triple stellar systems.
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: Possible orbits of a planet in a hierarchical triple-star system. Note that m 1, m 2, and m 3 do not necessarily agree.
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: Same as Figure 2, but for R.A. between 12 and 24 hr. Some of the system names for objects at or near the Summer Triangle have been omitted owing to overcrowding.
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: Summary of planetary types; see main text for references. For some planets, ambiguity exists regarding the planetary types. In this case, double listing has been chosen with the areas hatched. See Figure 4 for the definitions of the acronyms.
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: Distance for the various planet-hosting star systems; see main text for references. See Figure 4 for the definitions of the acronyms.
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: Discovery method for the various exoplanets; see main text for references. See Figure 4 for the definitions of the acronyms.
Paper: A Generalized Phase Diversity Technique Using Multiple Defocused Images
Authors: F. J. Bailén, D. Orozco Suárez, J. Blanco Rodríguez, J. C. del Toro Iniesta
Figure caption: The top panel shows the Zernike coefficients (in wavelength units) of the true incident wave front (black solid) and the retrieved coefficients for different symmetric choices of the phase diversities: K = 2 (dashed red), K = 3 (dashed–dotted blue), K = 5 (dashed green), K = 7 (dotted magenta), and K = 9 (dotted cyan). The bottom panel shows a residual of the fitting of the Zernike coefficients displayed in the top panel.
Paper: A Generalized Phase Diversity Technique Using Multiple Defocused Images
Authors: F. J. Bailén, D. Orozco Suárez, J. Blanco Rodríguez, J. C. del Toro Iniesta
Figure caption: Focused object (a), original MHD simulation (b), restored objects using K = 2, 3, 5, 7, 9 ((c), (e), (g), (i), (k)), and residual of the restored object compared to the original MHD simulation ((d), (f), (h), (j), (l)). The focused and the restored scenes have been normalized to the average continuum intensity of the quiet Sun, I QS. Values in the frames correspond to the contrasts (left column) and rms of the residuals (right column).
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 g-band light curves of NGC 5548's comparison star observed by ASAS-SN in 2018, 2019, 2020, and 2021. The scatter of the light curves is 0.04 mag (i.e., 4%), which is comparable to the average photometric uncertainty of 0.03 mag. The V-band light curves observed by ASAS-SN in 2015 are not included.
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: Phase diverse defocus that produces the best wave front retrieval, Δopt, for each value of J (blue) and the rms error of the Zernike fitting (red). The number of Zernike polynomials that describe the incident wave front coincides in this case with that of the retrieved one: J = J ab. The top panel corresponds to a λ/5 incident wave front. The bottom panel shows the results for a λ/10 wave front.
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 S/N = 1000. 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: 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) High-contrast MHD simulation showing two solar pores. (b) Focused image obtained after degrading (a) with the λ/5 rms wave front and adding noise. (c) Defocused image obtained as in (b) and 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: 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: Optimal value of Δ for the scene shown in Figure 6. Rms error of the Zernike coefficients fitting f as a function of Δ. Each curve represents different experiments with different values of J.
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: Comparison on IRASF10038-3338 between the physical properties inferred by Prospector and our SED fitting code. Left: resulting maps obtained with both codes, of the estimated A  V  (top), the SFRD (middle), and the SMD (bottom). Right: scatter plots of each physical property, with our SED fit inferred parameters on the x-axis, and the comparison (difference for A  V  and ratio for SMD and SFRD) of the Prospector and SED fit properties on the vertical axis. Each point corresponds to an individual bin of IRASF10038-3338. The black line and shaded region indicate the running median and standard deviation, respectively. Both qualitatively and quantitatively, the SMD seems the most robust parameter.
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: Infrared luminosity as a function of the redshift for the galaxies where L IR is available, as tabulated in Tables 1 and 3. The targets from the GOALS sample are indicated with the diamond markers (as opposed to white circles). The X-ray-selected AGNs are blue colored, whereas the non-AGNs are red. The inset plot shows the SFRIR (derived from L IR using Equation (6)) vs. the stellar mass (inferred with our SED fitting code), with the z = 0.02 main sequence from Whitaker et al. (2012) indicated as the dashed line.
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: Example of our SED fitting code applied on galaxy NGC 1614. The bottom right cutout shows the RGB image built combining the F435W, F814W, and F110W broadband filters. The top right plot shows the resulting SED fit on an example bin from the galaxy. The red points and uncertainties correspond to the original HST photometry. The blue crosses are the resulting synthetic photometry of the best fit. The black curve shows the best-fit resulting SED, which is a combination of the different colored continuum templates and the two line emission templates. The bottom panel shows the residual χ from the fit. On the left, we display the corner plot for the whole fit parameter space for this example bin, displaying the different correlations and distributions between the physical parameters that our code infers.
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: Comparison of the resulting Hα flux with a simple background subtraction method (top panel, interpolating two broadband filters) and our full SED machinery (bottom panel), on galaxy MCG-02-01-051. The vertical axis shows the logarithm of the ratio between each HST subtraction method inferred line estimates, and the reference MUSE Hα of this source. The SED fit Hα matches the MUSE one better than the commonly used simple subtraction method. The running median and uncertainty are shown as a solid black line and surrounding shaded region, respectively.
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: Voronoi binning for targets MCG-02-01-051 (top panels) and NGC 1614 (bottom panels). From left to right: original HST narrowband image that targets Paβ; binning on the narrowband image where we impose an S/N threshold of 20; Voronoi binning pattern, where the color map separates each individual bin from its neighbors; resulting signal-to-noise maps on the narrowband image after binning.
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: Transmission of some of the HST filters that cover our sample, indicated by the colored solid lines and the name for each filter, taken from the Spanish Virtual Observatory Filter Profile Service (Rodrigo & Solano 2020). The solid gray line corresponds to a galaxy SED redshifted to z = 0.03. The dashed turquoise line corresponds to a slope spectrum model used to fit the continuum in the ‘simple’ approach. The position of the Hα and Paβ emission lines are indicated by the colored narrow bandpasses.
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: Histogram (top left inset plot) and spatial map (main plot) of the [N II]/Hα ratio for MCG-02-01-051 as measured in the MUSE IFU cube. The value we adopt for the ratio (black dashed line on the histogram) falls within 1σ of the mean (gray shaded region).
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: Comparison between the Paβ inferred from our SED fitting scheme and the scaled F130N off-band subtraction for each spatial bin. The running median and scatter are shown as a solid black line and surrounding shaded region, respectively.
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 Hα+[N II] line flux for target MCG-02-01-051 inferred from the HST images with our SED fitting code (left), and the Hα+[N II] emission measured from the MUSE IFU cube (right) of the same source.
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: Extinction-corrected SFR﹩{}_{\mathrm{Paschen}}^{\mathrm{corr}}﹩ as a function of the SFR inferred from the infrared luminosity. The various data sets are detailed in the main text. Our sample is indicated by the diamond symbol, blue colored if they host an AGN and red colored if not.
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: Comparison of the spatially resolved SFRD inferred from Hα vs. from Paβ for galaxy MCG-02-01-051. The dashed line indicates the one-to-one ratio. The solid black line and shaded region indicate the running median and standard deviation, respectively. Top: SFRDs estimated from the observed Hα and Paβ, without correcting for dust extinction. Bottom: dust-corrected SFRDs, using the Balmer decrement (Hα/Hβ), obtained from the MUSE cube.
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: Comparison of the spatially resolved SFRDs inferred from stellar continuum versus from the dust-corrected Paβ. The dashed line indicates the one-to-one ratio. The color code indicates the stellar continuum A  V . Top: for target MCG-02-01-051. Bottom: for the targets in our sample that are part of GOALS. The black line and shaded region indicate the running median and standard deviation, respectively.
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: Extinction-corrected ﹩{{\rm{S}}{\rm{F}}{\rm{R}}}_{{\rm{P}}{\rm{a}}{\rm{s}}{\rm{c}}{\rm{h}}{\rm{e}}{\rm{n}}}^{{\rm{c}}{\rm{o}}{\rm{r}}{\rm{r}}}﹩ as a function of the SFR inferred from the 24 μm continuum emission. The various data sets are detailed in the main text. Our sample is indicated by the diamond symbol, blue colored if they host an AGN and red colored if not.