adsabs/AstroCLIMB huggingface dataset:
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Examples of six galaxies identified by the code as grand design and confirmed by eye. The first picture of each galaxy is the GZ-3D mask, the second picture is the SDSS g-band image. The two green contours on the GZ-3D masks correspond to one and three counts. The magenta ellipses show the inner and outer radii of the largest continuous radial range marked as two-armed by our software. The red circle indicates the center of the galaxy as marked by GZ-3D participants. On the SDSS g-band images, the same circle and ellipses are overlaid. In order left to right, top to bottom, the galaxies are as follows: MaNGA ID 1-1811 = IAU J101927.42-000204.3; MaNGA ID 1-32942 = IAU J010650.99-003413.7; MaNGA ID 1-260943 = IAU J141031.43 + 385353.8; MaNGA ID 1-555127 = IAU J023421.64-075224.2; MaNGA ID 1-567320 = IAU J094120.45 + 211656.9; and MaNGA ID 1-605134 = IAU J081752.00 + 125350.9. The white scale bars are 10″.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Examples of six galaxies identified by the code as multiarmed and confirmed by eye. The first picture of each galaxy is the GZ-3D mask, the second picture is the SDSS g-band image. The two green contours on the GZ-3D masks correspond to one and three counts. The magenta ellipses show the inner and outer radii of the largest continuous radial range marked as three-armed by our software. The red circle indicates the center of the galaxy as marked by GZ-3D participants. On the SDSS g-band images, the same circle and ellipses are overlaid. In order left to right, top to bottom, the galaxies are as follows: MaNGA ID 1-30797 = IAU J001039.34-000310.3; MaNGA ID 1-104906 = IAU J014636.04-085944.3; MaNGA ID 1-397480 = IAU J124727.84 + 403359.6; MaNGA ID 1-604111 = IAU J033758.99-061611.9; and MaNGA ID 1-638560 = IAU J121744.69 + 131029.9. The white scale bars are 10″.
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: histograms of the Yu & Ho (2020) pitch angle for galaxies in our multiarmed galaxies (red hatched) and our grand design galaxies (blue). Right: histograms of the GZ2 vote fraction for two arms (top panel) and for either three arms, four arms, five-plus plus arms, or ‘can't count arms’ (bottom panel) for galaxies in our grand design sample (blue) and our multiarmed sample (red hatched). Only “secure spirals” according to the definition of Hart et al. (2016) Hart et al. (2016) that have at least 20 classifications in GZ2 are included in the histograms on the right.
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: histograms of the Yu & Ho (2020) f3 parameter for our multiarmed galaxies (red hatched) and grand design galaxies (blue). Right: histograms of the Yu & Ho (2020) arm strengths for our multiarmed (red) and grand design (blue) 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: Plot of R50 vs. stellar mass for our multiarmed (red) vs. grand design galaxies (blue), as in Figure 5. Results from other studies are overlaid. See text for details.
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: histograms of R(max) divided by R90, where R90 is the radius enclosing 90% of the light. Right: histograms of the NSA ellipticities for the multiarmed galaxies (red hatched) and grand design galaxies (blue).
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: The fraction of the z < 0.05 GZ-3D galaxies in our final samples of multiarmed galaxies (red filled triangles) and grand design galaxies (blue open squares), as a function of concentration (left panel) and TType (right panel). The uncertainties are ﹩\sqrt{N}﹩.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: The fraction of the z < 0.05 GZ-3D galaxies in our final samples of multiarmed galaxies (red filled triangles) and grand design galaxies (blue open squares), as a function of stellar mass (left) and ellipticity (right). The uncertainties are ﹩\sqrt{N}﹩.
Paper: Automatic Search for Low-surface-brightness Galaxies from Sloan Digital Sky Survey Images Using Deep Learning
Authors: Zengxu Liang, Zhenping Yi, Wei Du, Meng Liu, Yuan Liu, Junjie Wang, Xiaoming Kong, Yude Bu, Hao Su, Hong Wu
Figure caption: The structure of GalCenterNet. The input image will be through ResNet50 and transposed convolution, and the obtained feature map will be input to the Heatmap module and Offset module to obtain the heatmap and offset values for the coordinates of the center point of the LSB galaxy. The final output of GalCenterNet is the coordinates of the center point of the LSB galaxy, derived from the heatmap corrected for the offset value.
Paper: Automatic Search for Low-surface-brightness Galaxies from Sloan Digital Sky Survey Images Using Deep Learning
Authors: Zengxu Liang, Zhenping Yi, Wei Du, Meng Liu, Yuan Liu, Junjie Wang, Xiaoming Kong, Yude Bu, Hao Su, Hong Wu
Figure caption: Three LSB galaxies are detected in an SDSS field image. The field image covers a sky area of 10′ by 13′ and 2048 by 1489 pixels.
Paper: Automatic Search for Low-surface-brightness Galaxies from Sloan Digital Sky Survey Images Using Deep Learning
Authors: Zengxu Liang, Zhenping Yi, Wei Du, Meng Liu, Yuan Liu, Junjie Wang, Xiaoming Kong, Yude Bu, Hao Su, Hong Wu
Figure caption: Four LSB galaxies and central coordinates from testing set. The center coordinates predicted by GalCenterNet are denoted by a blue “x,” while those predicted by YOLOv5 are represented by a red “x.” The central coordinates given by SDSS are indicated with a green “x.”
Paper: Automatic Search for Low-surface-brightness Galaxies from Sloan Digital Sky Survey Images Using Deep Learning
Authors: Zengxu Liang, Zhenping Yi, Wei Du, Meng Liu, Yuan Liu, Junjie Wang, Xiaoming Kong, Yude Bu, Hao Su, Hong Wu
Figure caption: Two LSB galaxies in an SDSS image. The LSB galaxies in red boxes are enlarged and displayed on the right side. The numbers in parentheses—i.e., (1263.90, 189.30)—represent the pixel coordinates of the LSB galaxies in the image.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Detection of the high-contrast companion HD 19467 B with the JWST NIRSpec IFU. (Left) Median spectral cube image from the JWST science calibration pipeline. (Middle) Detection map representing the companion S/N at each sky coordinate. The S/N is calculated using a joint FM of the starlight and the companion signal in the detector images, which can be compared to a cross-correlation S/N. HD 19467 B is detected with S/N = 232 after combining all exposures. (Right) Detection sensitivity (5σ) expressed as a companion-to-star flux ratio of various detection methods: FM, RDI, and the published ADI+RDI NIRCam F444W sensitivity from Carter et al. (2023) as the black line. We scaled the NIRCam contrast curve with the square root of the exposure time and stellar brightness to match the NIRSpec data set, although we note that the NIRCam detection limits have not yet been shown to be photon noise limited at small projected separations. The scatter in the NIRSpec detection limits do not represent its uncertainty, but they are the results of the 2D spatial variations of the NIRSpec PSF. The region within 0.″3 is grayed out because the current implementation of the method is not valid there, but it may theoretically be achieved in the future. The scatter plot of the PSF profile (gray) represents the raw PSF intensity values in each spaxel relative to the peak. In this plot, we demonstrate that the NIRSpec IFU reaches deep high-contrast sensitivity (10−6–10−5) at a small projected separation (0.″3–2″) with moderate-resolution spectroscopy.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Spectrum of HD 19467 B after RDI and WebbPSF spectral extraction (Section 5). The RDI flux error is shown as the blue-shaded region, which is estimated from the standard deviation of residual speckles spectra in an annulus around the companion. These errors are in practice correlated, so we conceptually separate the noise into two terms: the noise correlated on small spectral scales from interpolations (<2 pixels) and the noise correlated on larger scales from residual speckles. The standard deviation of the small-scale fraction of the total variance is labeled as the small-scale error. The photometry derived from the NIRSpec RDI spectrum is consistent with our reanalysis of the NIRCam photometry originally presented in Greenbaum et al. (2023) as well as the Lp data point from Maire et al. (2020) within calibration systematic uncertainties.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Spectrum of the A0 standard star TYC 4433-1800-1. The data come from the photometric calibration program 1128 with a four-point nod. For each wavelength range, the three panels, respectively, include from top to bottom: the spectral extraction featured in this work, a spectral cube-based extraction, the difference between the two methods, and a reference photometric calibration. (Top) The spectrum labeled “free centroid” is extracted by fitting the centroid and amplitude of a model PSF from WebbPSF to a 2D point cloud at each wavelength. “fixed centroid” means that only the flux was fitted for and the centroid was fixed to its median value in each detector. The “Fixed centroid - Corrected” spectrum was scaled by a linear trend to match the reference CALSPEC spectrum of TYC 4433-1800-1 (Bohlin et al. 2014; Bohlin & Lockwood 2022). (Middle) We show an updated extraction of the spectrum of TYC 4433-1800-1 originally published in Miles et al. (2023) obtained in private communication from the high-contrast ERS collaboration. This spectrum was extracted using aperture photometry of the spectral cubes built by the JWST science calibration pipeline. The WebbPSF-extracted spectrum remains impacted by the spatial undersampling at the shortest wavelengths. Future improvements in the calculation of the PSF model should improve these systematic errors. (Bottom) Difference of each spectrum with the CALSPEC spectrum.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Empirical derivation of a continuum-normalized spectrum of the host star HD 19467. This corresponds to a single exposure (jw01414004001_02101_00001_nrs2_cal.fits) with an integration time of 233.4 s of the NRS2 NIRSpec detector. For clarity, the third panel from the top zooms in a narrow interval of the wavelength highlighted in red. The wavelength bins δ λ are defined such that λ/δ λ ∼ 10,000.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Fitting a simulated PSF from WebbPSF to the 2D point cloud. (Left) Data at a fixed wavelength: 4.7 μm. The scatter plot indicates the spatial sampling of the point-cloud data being fitted. The image is a linear interpolation of the 2D point cloud only used for visualization purposes. The data itself is not interpolated in the fitting routine. (Middle Left) Image of the supersampled model PSF that is sampled onto the 2D point cloud of the science data. Unlike the data, the PSF model is interpolated in the fitting routine, which is fine because the model is numerically well sampled. (Middle right) Linear interpolation of the 2D point-cloud residuals: data minus best-fit model. (Right) Illustration of the 2D point cloud as a function of the declination showing the data, model, and residuals. The residuals were offset for clarity. This is data of the A0 star TYC 4433-1800-1 (program 1128) with a four-point nod.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Nonuniform spatial sampling after combining multiple dithers, due to interactions between the IFU slice offsets and the dither pattern offsets. Compare with Figure 5 right panel which shows the spatial sampling of a single dither position. (Upper left) Example of spatial sampling after combining a 4-point nod at 4.25 μm. This is the photometric standard data set featuring TYC 4433-1800-1 (program 1128). (Upper Right) Illustration of the different sampling for the same data set at 5 μm. (Bottom panels) Similar illustrations for the HD 19467 science data set presented in this work with nine dithers from the small cycling pattern.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Interpolation of a NIRSpec detector image onto a regular wavelength grid (jw01414004001_02101_00001_nrs2_cal.fits). (Left) Original flux-calibrated detector image featuring the slices of the NIRSpec IFU. The slices around the saturated star are masked. (Middle) Interpolated image where each column is at a constant wavelength. (Right) Spatial sampling (2D point cloud) of a vertical cut of the interpolated image.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Illustration of the data processing steps showing conceptually the information flow between the complementary techniques used. Section 3 describes the processing and reduction of uncalibrated (uncal) data, for both science and reference targets. The point-cloud results from combining flux-calibrated detector images (cal) with the corresponding spatial (R.A., decl.) and spectral (λ) coordinates of each pixel. The output spectral information from Section 3 flows into both the FM, described in Section 4, and the RDI PSF subtraction, described in Section 5. The outputs of the FM are the flux, S/N, and detection sensitivity maps. The output of the RDI PSF subtraction is the companion spectrum. Section 6 presents steps toward more tightly integrating these methods through the use of RDI outputs to set priors on the FM.
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: Distribution of the distances between all possible pairs in a imaging polarimetric frame. The two peaks correspond to the distance between the ordinary and extraordinary sources in the image. The image and the corresponding found pairs can be found in Figure 4. The orange and blue distributions correspond to the distances in the X- and Y-axis, respectively. The image corresponds to a CAFOS photo-polarimetric observation of the BL Lacertae field.
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: Paired sources in an example of CAFOS imaging polarimetric observation of the BL Lacertae field. The distance used for pairing was obtained from Figure 3. The resulting calibrated image can be found in Figure 5. Ordinary and Extraordinary sources are circled with the same color.
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: DIPOL polarimetry (left) and photometry (right) frames of BL Lacertae observations. Only the shown subframe (2.′5 × 2.′0 ) is usually saved to disk during polarimetric observations with DIPOL, which prevents blind solving of the image. The full photometry field (9.′2 × 6.′3) is saved, however, and the correspondence between both images can be found by comparing quads of sources through a hashing algorithm. This allows us to automatically distinguish the O and E images of our target source in the field.
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: Database schema of IOP4. ForeignKey relationships relate one or several instances of model A to a single instance of model B. In ManyToMany relationships, multiple instances of model A and B are linked together. The latter does not show a field in the tables of this diagram, since the relationship is established through a hidden table omitted here. Some fields of the AstroSource model have been also omitted to save space (corresponding to literature magnitudes in other bands, e.g., mag_B, etc). An arrow in any direction signify multiple instances being linked to the origin (e.g., several RawFit(s) are linked to one Epoch).