adsabs/AstroCLIMB huggingface dataset:
Paper: IOP4, the Interactive Optical Photo-Polarimetric Python Pipeline
Authors: Juan Escudero Pedrosa, Iván Agudo, Daniel Morcuende, Jorge Otero-Santos, Giacomo Bonnoli, Vilppu Piirola, César Husillos, Mabel Bernardos, Rubén López-Coto, Alfredo Sota, Victor Casanova, Fran J. Aceituno, Pablo Santos-Sanz
Figure caption: Different ways of interacting with IOP4. The pipeline (through the IOP4 command, Python script or Jupyter notebooks) can directly interact with the data aided by IOP4LIB. The IOP4API application exposes a series of API end points that allow the client to authenticate itself, query, plot and flag data, and explore catalog and logs from a web browser through a single-page application (SPA). The IOP4ADMIN site independently provides a way to interact and edit all models in the database.
Paper: IOP4, the Interactive Optical Photo-Polarimetric Python Pipeline
Authors: Juan Escudero Pedrosa, Iván Agudo, Daniel Morcuende, Jorge Otero-Santos, Giacomo Bonnoli, Vilppu Piirola, César Husillos, Mabel Bernardos, Rubén López-Coto, Alfredo Sota, Victor Casanova, Fran J. Aceituno, Pablo Santos-Sanz
Figure caption: Calibrated CAFOS photo-polarimetric image of the BL Lacertae field. The positions of the ordinary image of BL Lacertae (labeled as 2200+420) and its calibrators (B, C, H) are indicated with a circle. The position of the extraordinary images are represented with an “x.”
Paper: IOP4, the Interactive Optical Photo-Polarimetric Python Pipeline
Authors: Juan Escudero Pedrosa, Iván Agudo, Daniel Morcuende, Jorge Otero-Santos, Giacomo Bonnoli, Vilppu Piirola, César Husillos, Mabel Bernardos, Rubén López-Coto, Alfredo Sota, Victor Casanova, Fran J. Aceituno, Pablo Santos-Sanz
Figure caption: Directory structure of the IOP4 local archive.
Paper: SuperBIT Superpressure Flight Instrument Overview and Performance: Near-diffraction-limited Astronomical Imaging from the Stratosphere
Authors: Ajay S. Gill, Steven J. Benton, Christopher J. Damaren, Spencer W. Everett, Aurelien A. Fraisse, John W. Hartley, David Harvey, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Richard Massey, Jacqueline E. McCleary, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, L. Javier Romualdez, Jürgen Schmoll, Mohamed M. Shaaban, Ellen L. Sirks, Georgios N. Vassilakis, André Z. Vitorelli
Figure caption: The SuperBIT inner frame mounted inside the middle frame. We highlight the subsystems mounted on the inner frame. This is a preflight image taken during the Wanaka integration campaign.
Paper: SuperBIT Superpressure Flight Instrument Overview and Performance: Near-diffraction-limited Astronomical Imaging from the Stratosphere
Authors: Ajay S. Gill, Steven J. Benton, Christopher J. Damaren, Spencer W. Everett, Aurelien A. Fraisse, John W. Hartley, David Harvey, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Richard Massey, Jacqueline E. McCleary, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, L. Javier Romualdez, Jürgen Schmoll, Mohamed M. Shaaban, Ellen L. Sirks, Georgios N. Vassilakis, André Z. Vitorelli
Figure caption: The SuperBIT gondola diagram, highlighting the three-frame system and the major instrument components.
Paper: SuperBIT Superpressure Flight Instrument Overview and Performance: Near-diffraction-limited Astronomical Imaging from the Stratosphere
Authors: Ajay S. Gill, Steven J. Benton, Christopher J. Damaren, Spencer W. Everett, Aurelien A. Fraisse, John W. Hartley, David Harvey, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Richard Massey, Jacqueline E. McCleary, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, L. Javier Romualdez, Jürgen Schmoll, Mohamed M. Shaaban, Ellen L. Sirks, Georgios N. Vassilakis, André Z. Vitorelli
Figure caption: The SuperBIT flight (728NT) track, showing five complete circumnavigations in green and the path of the final 3 days in red (credit: NASA Columbia Scientific Balloon Facility).
Paper: SuperBIT Superpressure Flight Instrument Overview and Performance: Near-diffraction-limited Astronomical Imaging from the Stratosphere
Authors: Ajay S. Gill, Steven J. Benton, Christopher J. Damaren, Spencer W. Everett, Aurelien A. Fraisse, John W. Hartley, David Harvey, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Richard Massey, Jacqueline E. McCleary, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, L. Javier Romualdez, Jürgen Schmoll, Mohamed M. Shaaban, Ellen L. Sirks, Georgios N. Vassilakis, André Z. Vitorelli
Figure caption: SuperBIT on the launch pad in Wānaka, New Zealand, for the 2023 superpressure flight on 2023 April 16 (credit: NASA Columbia Scientific Balloon Facility / Bill Rodman).
Paper: SuperBIT Superpressure Flight Instrument Overview and Performance: Near-diffraction-limited Astronomical Imaging from the Stratosphere
Authors: Ajay S. Gill, Steven J. Benton, Christopher J. Damaren, Spencer W. Everett, Aurelien A. Fraisse, John W. Hartley, David Harvey, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Richard Massey, Jacqueline E. McCleary, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, L. Javier Romualdez, Jürgen Schmoll, Mohamed M. Shaaban, Ellen L. Sirks, Georgios N. Vassilakis, André Z. Vitorelli
Figure caption: Atmospheric transmission as a function of altitude.
Paper: SuperBIT Superpressure Flight Instrument Overview and Performance: Near-diffraction-limited Astronomical Imaging from the Stratosphere
Authors: Ajay S. Gill, Steven J. Benton, Christopher J. Damaren, Spencer W. Everett, Aurelien A. Fraisse, John W. Hartley, David Harvey, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Richard Massey, Jacqueline E. McCleary, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, L. Javier Romualdez, Jürgen Schmoll, Mohamed M. Shaaban, Ellen L. Sirks, Georgios N. Vassilakis, André Z. Vitorelli
Figure caption: The overall SuperBIT bandpasses. SuperBIT’s main science bands were u, b, and g for the weak-lensing observations of galaxy clusters.
Paper: SuperBIT Superpressure Flight Instrument Overview and Performance: Near-diffraction-limited Astronomical Imaging from the Stratosphere
Authors: Ajay S. Gill, Steven J. Benton, Christopher J. Damaren, Spencer W. Everett, Aurelien A. Fraisse, John W. Hartley, David Harvey, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Richard Massey, Jacqueline E. McCleary, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, L. Javier Romualdez, Jürgen Schmoll, Mohamed M. Shaaban, Ellen L. Sirks, Georgios N. Vassilakis, André Z. Vitorelli
Figure caption: The various electronics modules installed on the SuperBIT outer frame. This is a preflight image taken during the Wanaka integration campaign.
Paper: SuperBIT Superpressure Flight Instrument Overview and Performance: Near-diffraction-limited Astronomical Imaging from the Stratosphere
Authors: Ajay S. Gill, Steven J. Benton, Christopher J. Damaren, Spencer W. Everett, Aurelien A. Fraisse, John W. Hartley, David Harvey, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Richard Massey, Jacqueline E. McCleary, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, L. Javier Romualdez, Jürgen Schmoll, Mohamed M. Shaaban, Ellen L. Sirks, Georgios N. Vassilakis, André Z. Vitorelli
Figure caption: The transmission of the individual components that comprise the SuperBIT bandpasses.
Paper: CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Adam E. Lanman, Shion Andrew, Mattias Lazda, Vishwangi Shah, Mandana Amiri, Arvind Balasubramanian, Kevin Bandura, P. J. Boyle, Charanjot Brar, Mark Carlson, Jean-François Cliche, Nina Gusinskaia, Ian T. Hendricksen, J. F. Kaczmarek, Tom Landecker, Calvin Leung, Ryan Mckinven, Juan Mena-Parra, Nikola Milutinovic, Kenzie Nimmo, Aaron B. Pearlman, Andre Renard, Mubdi Rahman, J. Richard Shaw, Seth R. Siegel, Rick J. Smegal, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Mark Halpern, Hans Hopkins, Victoria M. Kaspi, Kholoud Khairy, Kiyoshi W. Masui, Bradley W. Meyers, Daniele Michilli, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick Smith, Keith Vanderlinde, Tarik J. Zegmott
Figure caption: The analog system from the antenna to the ADC. The antenna feed and LNA are contained in an enclosed cassette on the focal line, which protects them from weather. Low-loss coaxial cable connects the cassette to the the exterior of the receiver hut, which feeds through to an inner bulkhead that holds the Mini-Circuits custom LTE filter. The LTE-filtered signal is then passed into the RF-shielded room, amplified by the FLA, and sampled.
Paper: CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Adam E. Lanman, Shion Andrew, Mattias Lazda, Vishwangi Shah, Mandana Amiri, Arvind Balasubramanian, Kevin Bandura, P. J. Boyle, Charanjot Brar, Mark Carlson, Jean-François Cliche, Nina Gusinskaia, Ian T. Hendricksen, J. F. Kaczmarek, Tom Landecker, Calvin Leung, Ryan Mckinven, Juan Mena-Parra, Nikola Milutinovic, Kenzie Nimmo, Aaron B. Pearlman, Andre Renard, Mubdi Rahman, J. Richard Shaw, Seth R. Siegel, Rick J. Smegal, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Mark Halpern, Hans Hopkins, Victoria M. Kaspi, Kholoud Khairy, Kiyoshi W. Masui, Bradley W. Meyers, Daniele Michilli, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick Smith, Keith Vanderlinde, Tarik J. Zegmott
Figure caption: Digital system configuration at KKO, picking up from where Figure 2 ended. Black boxes indicate separate computing nodes, with the node name in the corner. Amplified antenna voltages are sampled and channelized in the F-engine into baseband data, which is buffered and correlated in the X-engine. The frequency standard from the Rubidium clock (“Rb clock”) is also sampled in the F-engine via one of the inputs. Visibility data are sent to c2, where they are used for gain calculation, and baseband data are sent to c1, where they are transposed and saved on triggers. The arc and aux nodes handle system management tasks, as well as forwarding triggers from CHIME.
Paper: CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Adam E. Lanman, Shion Andrew, Mattias Lazda, Vishwangi Shah, Mandana Amiri, Arvind Balasubramanian, Kevin Bandura, P. J. Boyle, Charanjot Brar, Mark Carlson, Jean-François Cliche, Nina Gusinskaia, Ian T. Hendricksen, J. F. Kaczmarek, Tom Landecker, Calvin Leung, Ryan Mckinven, Juan Mena-Parra, Nikola Milutinovic, Kenzie Nimmo, Aaron B. Pearlman, Andre Renard, Mubdi Rahman, J. Richard Shaw, Seth R. Siegel, Rick J. Smegal, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Mark Halpern, Hans Hopkins, Victoria M. Kaspi, Kholoud Khairy, Kiyoshi W. Masui, Bradley W. Meyers, Daniele Michilli, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick Smith, Keith Vanderlinde, Tarik J. Zegmott
Figure caption: A waterfall plot showing autocorrelation for a single input over 24 hr. The solar transit can be clearly seen at 20:04 UTC. The bottom panel shows the mean over time. The LTE band is distinguishable between 710 and 760 MHz, with a vertical stripe of missing data where the gain calculation failed to converge. No masking has been applied here, but the LTE band, the region around 630 MHz, and a few narrow lower-frequency channels are all removed from analysis using a static frequency mask (see Section 3.2).
Paper: CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Adam E. Lanman, Shion Andrew, Mattias Lazda, Vishwangi Shah, Mandana Amiri, Arvind Balasubramanian, Kevin Bandura, P. J. Boyle, Charanjot Brar, Mark Carlson, Jean-François Cliche, Nina Gusinskaia, Ian T. Hendricksen, J. F. Kaczmarek, Tom Landecker, Calvin Leung, Ryan Mckinven, Juan Mena-Parra, Nikola Milutinovic, Kenzie Nimmo, Aaron B. Pearlman, Andre Renard, Mubdi Rahman, J. Richard Shaw, Seth R. Siegel, Rick J. Smegal, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Mark Halpern, Hans Hopkins, Victoria M. Kaspi, Kholoud Khairy, Kiyoshi W. Masui, Bradley W. Meyers, Daniele Michilli, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick Smith, Keith Vanderlinde, Tarik J. Zegmott
Figure caption: Using the solar transit on 2023 June 6 to map the primary beam vs. frequency. The values depicted are the mean autocorrelation (mean taken over input), normalized to the values at 0 hr angle. The HA reported is with respect to the CHIME meridian, since the KKO dish is rolled and rotated so that its axis aligns with CHIME’s.
Paper: CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Adam E. Lanman, Shion Andrew, Mattias Lazda, Vishwangi Shah, Mandana Amiri, Arvind Balasubramanian, Kevin Bandura, P. J. Boyle, Charanjot Brar, Mark Carlson, Jean-François Cliche, Nina Gusinskaia, Ian T. Hendricksen, J. F. Kaczmarek, Tom Landecker, Calvin Leung, Ryan Mckinven, Juan Mena-Parra, Nikola Milutinovic, Kenzie Nimmo, Aaron B. Pearlman, Andre Renard, Mubdi Rahman, J. Richard Shaw, Seth R. Siegel, Rick J. Smegal, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Mark Halpern, Hans Hopkins, Victoria M. Kaspi, Kholoud Khairy, Kiyoshi W. Masui, Bradley W. Meyers, Daniele Michilli, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick Smith, Keith Vanderlinde, Tarik J. Zegmott
Figure caption: The KKO site. Top: photo of KKO and its site. This photo was taken during servicing, with the service trolley occupied and shifted over the cylinder. During normal operations, the trolley is kept by the scaffolding to the right. Bottom: map showing the KKO geographic location relative to CHIME and nearby population centers. North is up. Satellite imagery ©2023 TerraMetrics, map data ©2023 Google.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Plots of the log of the sSFR vs. log M *. The left panels show the positions of individual galaxies, with grand design galaxies in the top panel and multiarmed galaxies in the bottom panel. In the panels on the left, the best-fit line for each subset and its parameters are shown in the corresponding color. The right panel gives the median sSFR for each subset as a function of log M *, within 0.3 dex bins in log M *. The sample is split into four subsets: blue open squares, grand design, NSA C ≥ 2.65; green crosses, grand design, NSA C < 2.65; red open triangles, three-armed, NSA C ≥ 2.65; black open circles, three-armed, NSA C < 2.65. In the right panel, the four subsets for a given log M * are slightly shifted along the x-axis for ease in viewing. The error bars in the right panel give the error in the median ∼IQR/﹩\sqrt{N}﹩, where IQR is the interquartile range and N is the number of data points in that set. Only for the low-C 9.5 ≤ log (M */M ☉) < 10 bin is there a marginally significant difference between the grand design and multiarmed galaxies, and only for the KS test.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Left: plot of concentration vs. stellar mass for galaxies in our multiarmed galaxy sample (red filled triangles) and galaxies classified as grand design (blue open squares). Concentration is defined as the ratio of R90/R50, where R90 and R50 are the radii containing 90% and 50% of the SDSS r-band light, respectively, using elliptical Petrosian radii from the NSA. The red line is the best fit for the multiarmed galaxies, while the blue line is the best fit for the grand design galaxies. The best-fit slope (m), y-intercept (b), and rms for the two sets of galaxies are displayed in the corresponding color, along with the Spearman (ρ) and Pearson (r) correlation coefficient. Right: plot of median concentration for the grand design galaxies (open blue squares) and the multiarmed galaxies (red filled triangles) in bins in log M *. The error bars give the error in the median ∼IQR/﹩\sqrt{N}﹩, where IQR is the interquartile range and N is the number of data points in that set. The red and blue data points are slightly offset from the center of the mass bin to make the data easier to see. Results of KS/AD tests comparing the grand design and the multiarmed galaxies in each mass bin are given in Table 1.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Histograms of the Domínguez Sánchez et al. (2018) Hubble type (TType) for our multiarmed (red hatched) and grand design galaxies (blue). The left axis gives the number of galaxies for the multiarmed sample, while the right axis gives the number of grand design galaxies. Right: plot of the Domínguez Sánchez et al. (2018) TType vs. log stellar mass for our multiarmed galaxies (red filled triangles) and grand design galaxies (blue open squares). The best-fit line for the multiarmed galaxies is plotted in red, while the best-fit line for the grand design galaxies is given in blue. The parameters of the best-fit line are given in the corresponding color.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Left: plot of log Σ1 vs. log M * for the multiarmed (red filled triangles) and grand design (blue open squares) galaxies. The red line is the best-fit line for the multiarmed galaxies; the blue line is the best-fit line for the grand design galaxies. The parameters of the fits are given in the corresponding colors. The green dotted curve is the Luo et al. (2020) dividing line between galaxies with classical bulges (above the curve) and pseudo-bulges (below). Right: log ΔΣ1 for multiarmed (red hatched) and grand design (blue) galaxies, where log ΔΣ1 is defined by Luo et al. (2020) as the offset from the green curve in the left panel. Galaxies that lie to the right of zero in these histograms lie above the green curve in the plot on the left. The left axis gives the number of galaxies for the multiarmed sample, while the right axis gives the number of grand design galaxies.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Left: plot of the log of the SDSS r-band R50 radius (half-light radius) from the NSA vs. the log of the stellar mass, for our multiarmed (red filled triangles) and grand design galaxies (blue open squares). Right: plot of R90, the radius containing 90% of the SDSS r-band light, vs. the stellar mass for our sample of multiarmed galaxies (red filled triangles) and the grand design galaxies (blue filled squares). The red lines are the best-fit linear relations for the multiarmed galaxies, while the blue lines are the best-fit lines for the grand design galaxies. The parameters of the best-fit lines and the Spearman (ρ) and Pearson (r) correlation coefficients are overlaid in the corresponding color.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Histograms of the concentrations for our multiarmed (red hatched) vs. grand design galaxies (blue). Concentration is defined as the ratio of R90/R50, where R90 and R50 are the radii containing 90% and 50% of the SDSS r-band light, respectively, using elliptical Petrosian radii from the NSA. The left axis gives the number of galaxies for the multiarmed sample, while the right axis gives the number of grand design galaxies.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Stellar mass vs. redshift for our grand design (blue open squares) and multiarmed galaxies (red filled triangles). Other galaxies in our initial set of 4449 GZ-3D galaxies with z < 0.05, ellipticity ≤0.5 are marked by small black dots. The galaxies in the “Primary” and “Secondary” MaNGA subsets are separated into two “bands” in this plot, with the larger-angular-size “Primary” galaxies in the leftmost band.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Histograms of redshifts (left panel) and stellar masses (right panel) for the final set of multiarmed galaxies (red hatched histogram) and grand design spirals (blue histogram). The left axis gives the number of galaxies for the multiarmed sample, while the right axis gives the number of grand design galaxies.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: Differences between fitted exponential color–metallicity and color–color relations, comparing PARSEC CMD 3.6 to the other four models (i.e., subtracting each model from PARSEC CMD 3.6). As in previous figures, PARSEC CMD 3.7 is shown in blue, BaSTI alpha-enhanced in orange, BaSTI solar-scaled in red, and MIST in pink; similarly, relations based on the (F475X–F110W) color index are shown as solid lines and relations based on the (F475W–F850LP) index as dashed lines.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: Model GCs from the PARSEC, BaSTI, and MIST SSPs. With all five models, we simulated GCs with metallicities ranging from −2.2 to 0.0 dex and ages ranging from 9 to 13 Gyr, and calculated integrated magnitudes in (F475X–F110W) and (F475W–F850LP). Top left: PARSEC CMD 3.6, the model used in Hartman et al. (2023). Top right: PARSEC CMD 3.7, the latest version of PARSEC available online as of the time of writing. Middle left: BaSTI’s α-enhanced model. Middle right: BaSTI’s solar-scaled model. Bottom left: MIST isochrone-derived model GCs.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: Left column: model GCs with fitted exponential metallicity–color relations overplotted. Points are colored as in Figure 1. Center column: residuals from the (F475X–F110W)–metallicity relations. Right column: residuals from the (F475W–F850LP)–metallicity relations.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: Ratio of metallicity uncertainty and color uncertainty by color index for each of the five stellar models and both color indices; see Equation (2). Color is a less sensitive tracer of metallicity at the blue end of color–metallicity space than at the red end.