adsabs/AstroCLIMB huggingface dataset:
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Same as Figure 3 but for Johnson–Cousins bands and using simulated measurement uncertainties of 0.1 magnitudes.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Same as Figure 3 but using simulated measurement uncertainties of 0.1 magnitudes.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Same as Figure 3 but for Johnson–Cousins bands.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Same as Figure 4 but for fits with uncertainties underestimated by a factor of two.
Paper: Errors When Constraining Hot Blackbody Parameters with Optical Photometry
Authors: Iair Arcavi
Figure caption: Differences in blackbody absolute magnitudes generated by the two packages used here (pysynphot and lightcurve_fitting) for various bands at various temperatures.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: NSO Carrington maps of the radial magnetic field during sunspot cycles 21–23 (top, middle, and bottom panels, respectively), showing flux streaming poleward and eastward from the sunspot belts during the initial phase of sunspot maximum (left panels) and flux accumulating in the equatorial region between the sunspot belts at the end phase of sunspot maximum (right panels). Longitude runs left to right from 0° to 360°, and sine latitude ranges from −1 to +1 from the bottom to top of each map. Positive polarity is white and negative is black. Dates refer to the starting times at the right edge of each map.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: WSO measurements of the Sun’s north (black) and south (blue) polar fields, superimposed on the smoothed plot of the B 0-induced part of the axisymmetric field (purple), and compared with the monthly averaged sunspot number (black). Annual variations of the purple curve are in phase with the annual variations of the polar fields, but the polar fields had to be divided by separate factors of 20 and 30 to improve the agreement between the long-term envelopes of these curves.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Top panel: twenty-seven day running average of the WSO mean field (red), compared with the monthly averaged sunspot number from SILSO (blue). Bottom panel: three-hundred sixty-five day moving average of the red curve, showing the residual ﹩{Y}_{2}^{0}﹩ component of the axisymmetric field (purple) after the annually varying ﹩{Y}_{1}^{0}﹩ and ﹩{Y}_{3}^{0}﹩ contributions have been removed.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Weighted sum of WSO north and south polar fields (blue), superimposed on the B 0-induced part of the axisymmetric field (purple), and compared with the monthly averaged sunspot number (black) during cycles 21–24. Annual variations of this sum approximately match those of the purple curve, except in the years around sunspot maximum when the polar fields reverse and the purple curve has large spikes.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Carrington maps, cropped to show northern-hemisphere magnetic fields as a function of longitude (0°–360° on the horizontal axis) and sine latitude (0 to +1 on the vertical axis). Left panel: CR1788-1795 (1987 April 22–October 30), showing the northward and eastward drift of flux from a new-cycle active region. Right panel: CR1811-1818 (1989 January 9–July 19), showing a stronger stream from a bigger active region near sunspot maximum. Faint yellow lines indicate a 30.2 day rotation.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: The axisymmetric field, 〈B  m 〉, with its ﹩{Y}_{2}^{0}﹩ component removed and a 75 day smoothing applied to the remainder. The resulting purple curve shows annular modulation, especially during the 1976, 1986, and 2019 sunspot minima. The black curve shows the monthly averaged sunspot number from SILSO.
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: Evolution of Hα-to-stellar continuum morphologies for star-forming galaxies between 0.5 ≲ z ≲ 1.7. Panel (A): stellar mass distributions of the data sets. Ratio of the Hα-to-stellar continuum effective radius R  eff  (panel (B)), surface density within the effective radius Σ eff  (panel (C)), and surface density within 1 kpc Σ1kpc (panel (D)) for CLEAR (z ∼ 0.5), 3D-HST (z ∼ 1), and KMOS3D (z ∼ 1.7). KMOS3D results are plotted as running means from individual measurements. Over the stellar mass range shown, the Hα-to-stellar continuum R  eff , Σ eff , and Σ1kpc are on average the same between 0.5 ≲ z ≲ 1.7 within 1σ (see Table 2). Trends of larger/more extended Hα than stellar continuum for higher-mass galaxies at fixed redshift and larger/more extended Hα for z ∼ 0.5 galaxies at fixed stellar mass are apparent for all three morphology parameters, but are stronger in Σ1kpc. Between 0.5 ≲ z ≲ 1, the slope of the ﹩\tfrac{{{\rm{\Sigma }}}_{1\mathrm{kpc},\,{\rm{H}}\alpha }}{{{\rm{\Sigma }}}_{1\mathrm{kpc},\mathrm{Cont}}}﹩–stellar mass relation is constant, but the intercept increases by a factor of 1.07 (see Table 3) between z ∼ 0.5 and z ∼ 1 (panel D). Shaded regions around the best-fit lines to the CLEAR and 3D-HST measurements show 68% confidence intervals. At log(M */M ⊙) = 9.5, star-forming galaxies at z ∼ 0.5 have a (19 ± 2)% lower surface density in Hα compared to the stellar continuum than z ∼ 1 star-forming galaxies within a galactocentric radius of 1 kpc.
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: Top row: stellar continuum and Hα stellar mass–size relations for CLEAR. Small markers show measurements on individual galaxies, larger markers show measurements from stacks. Shaded gray regions delineate the stellar mass bins for each stack. Sample sizes for the stacks and individual measurements (in brackets) are stated at the bottom for each bin. The region enclosed by the van der Wel et al. (2014) z = 0.25 and z = 0.75 mass–size relations (sizes measured at rest-frame wavelength of 5000 Å) are shown as the red shaded region. Effective radii for all measurements shown are not circularized. A typical 1σ error on individual measurements from van der Wel et al. (2014) is shown as the black error bar in the top right of each panel. Bottom row: ratio of the Hα-to-stellar continuum effective radius. The thick gray line shows a running median for the individual fits. On average, the Hα effective radius is 1.2 ± 0.1 times larger than the effective radius of the stellar continuum at fixed stellar mass. Particularly large Hα effective radii are seen both in the individual and stack measurements at log(M */M ⊙) ∼ 9.5 for all fields excluding GS4. See Section 6.1 for more details.
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: Normalized surface brightness profiles of the CLEAR stellar continuum and Hα stacks along with their GALFIT models and PSFs. GALFIT results for effective radii are marked with short vertical lines. GALFIT results for Sérsic indices are stated in the top-right-hand corner of each subplot. In general, GALFIT does a good job of measuring the shape of the stellar continuum and Hα surface brightness profiles out to ∼10 kpc. The stellar continuum is always more compact than the Hα emission when comparing the stellar mass surface density within 1 kpc, Σ1kpc. This trend breaks down when relying on Sérsic index, n, as a proxy for compactness, where Hα seems to be more compact than the stellar continuum in one case (second panel). This reflects a degeneracy between n and R  eff . See Section 6.2 for more details.
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: The ratio of the Hα-to-stellar continuum stellar mass surface density within various galactocentric radii, Σ r . r = 5 kpc represents the approximate maximum effective radius measured in the three data sets. Σ1 kpc (dark purple lines) exhibits the strongest trend with stellar mass for all three data sets. Σ r  at smaller galactocentric radii are more reliable since they probe the highest S/N and therefore most well-determined parts of the stellar continuum and Hα light profiles (see Figure 8 and Section 6.4 for more details).
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: Zoomed-in regions (89 × 89 pixels, pixel scale = 0.″1) of the F105W (stellar continuum) and Hα stacks for the CLEAR sample with their associated GALFIT fits. Original thumbnails are 189 × 189 pixels (see Section 3.1.4 for reasoning). The mean grism redshift (﹩\overline{z}﹩) of each stack is stated along with the log(M */M ⊙) range of each stack in square brackets. The color map is logarithmic, with Hα stacks and fits multiplied by 100 for visibility.
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: Grism redshift (left panel) and stellar mass (right panel) distributions for galaxies in the CLEAR sample used in this study. The primary sample (279 galaxies) shows the galaxies that go into the stacks. Individual fits (97 galaxies) show the distributions for those galaxies that obtained good-quality individual fits.
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: Level of agreement with results from van der Wel et al. (2012) for the F105W effective radii of the same galaxies from individual fits shown in Figure 7. Only measurements that had good-quality fits (flag value = 0) in the van der Wel et al. (2012) catalogs are shown. Solid black line indicates the position of one-to-one agreement between the two size determination methods. Our sizes are on average 0.4% smaller than those of van der Wel et al. (2012).
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption:  UVJ color separation (solid black line) applied to our sample to select star-forming galaxies during the sample selection process. See Section 3.2.1 for details. Background contours show the full photometrically selected sample between 0.22 ≲ z ≲ 0.75 and log(M */M ⊙) ≥ 8.96. Markers show all galaxies in CLEAR that pass the first three steps of sample selection (see Table 1) with stellar masses Log(M */M ⊙) ≥ 8.96.
Paper: CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps
Authors: Jasleen Matharu, Casey Papovich, Raymond C. Simons, Ivelina Momcheva, Gabriel Brammer, Zhiyuan Ji, Bren E. Backhaus, Nikko J. Cleri, Vicente Estrada-Carpenter, Steven L. Finkelstein, Kristian Finlator, Mauro Giavalisco, Intae Jung, Adam Muzzin, Erica J. Nelson, Annalisa Pillepich, Jonathan R. Trump, Benjamin Weiner
Figure caption: Figure 1 continued.
Paper: Investigating the Asymmetry of Magnetic Field Profiles of “Simple” Magnetic Ejecta through an Expansion-modified Flux Rope Model
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Florian Regnault, Antoinette Galvin
Figure caption: The scatter distributions of the χ 2 values of the two models: (a) normalized χ 2 of the B components; (b) normalized ﹩{\chi }_{{B}_{{total}}}^{2}﹩; (c) DiP vs. normalized χ 2 of the B components; (d) DiP vs. normalized ﹩{\chi }_{{B}_{{total}}}^{2}﹩; (e) B ratio vs. normalized ﹩{\chi }_{{B}_{{total}}}^{2}﹩; and (f) S/A vs. normalized ﹩{\chi }_{{B}_{{total}}}^{2}﹩.
Paper: The Relation between the Optical Fe II Emission and the Dimensionless Accretion Rate for Active Galactic Nuclei
Authors: Yan-Sheng Liu, Wei-Hao Bian
Figure caption: Distributions of R Fe and L 5100 for the subsample of 4037 SDSS quasars (top panels, blue) and the subsample of 120 RM AGN (bottom panels, red). The dashed lines are their mean values. The number, the mean value, and the standard deviation are shown in panels.
Paper: Investigating the Asymmetry of Magnetic Field Profiles of “Simple” Magnetic Ejecta through an Expansion-modified Flux Rope Model
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Florian Regnault, Antoinette Galvin
Figure caption: Scatter distributions of the output parameters of the two models: (a) latitude angle, θ (°); (b) longitude angle, ϕ (°); (c) B 0 (nT) on the axis; (d) fitted radius (au); (e) α R of the Lundquist model vs. α R of the Exp-Lundquist model (front boundary); and (f) α R of the Lundquist model vs. α R/τ of the Exp-Lundquist model (rear boundary). Red indicates Type 1 MEs (13 events), blue indicates Type 2 MEs (two events), and green indicates Type 3 MEs (10 events). For each plot, the best-fit linear relation between the parameter is provided.
Paper: The Relation between the Optical Fe II Emission and the Dimensionless Accretion Rate for Active Galactic Nuclei
Authors: Yan-Sheng Liu, Wei-Hao Bian
Figure caption: Distributions of FWHM H β , σ Hβ , and their ratio FWHM H β /σ Hβ  for the broad H β. The blue lines are for the subsample of 4037 SDSS quasars. The red lines are for the subsample of 120 RM AGN. The fractional numbers are used to compare the distributions for two subsamples.
Paper: The Relation between the Optical Fe II Emission and the Dimensionless Accretion Rate for Active Galactic Nuclei
Authors: Yan-Sheng Liu, Wei-Hao Bian
Figure caption: Distributions for M BH and ﹩\dot{{\mathscr{M}}}﹩ derived from σ Hβ  (top two panels) and FWHM H β  (bottom two panels) for the subsample of 4037 SDSS quasars (blue) and the subsample of 120 RM AGN (red). The dashed lines are mean values. The number, the mean value, and the standard deviation are shown in panels.
Paper: Investigating the Asymmetry of Magnetic Field Profiles of “Simple” Magnetic Ejecta through an Expansion-modified Flux Rope Model
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Florian Regnault, Antoinette Galvin
Figure caption: STEREO-B: 2012 July 4 17:00:00–2012 July 5 12:50:00 (Type 3). The same format as Figure 1, but the magnetic field data are in RTN coordinates.
Paper: Investigating the Asymmetry of Magnetic Field Profiles of “Simple” Magnetic Ejecta through an Expansion-modified Flux Rope Model
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Florian Regnault, Antoinette Galvin
Figure caption: The expansion rate (ζ) of the Exp-Lundquist model and its relationships to the expansion speed and the goodness of fit.
Paper: Investigating the Asymmetry of Magnetic Field Profiles of “Simple” Magnetic Ejecta through an Expansion-modified Flux Rope Model
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Florian Regnault, Antoinette Galvin
Figure caption: The t 0 of the Exp-Lundquist model.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: Host galaxy properties. Panels (a)–(d): distributions of host galaxy stellar mass, redshift, absolute g-band magnitude, and g − r color. The [N II]/Hα-selected AGN candidates are shown as hashed teal histograms, the He II/Hβ-selected AGNs are plotted as brown histograms, the [Fe X] AGNs galaxies are shown as cross-hashed black histograms, and the [Ne V]-AGNs are shown as green histograms. Our parent sample of low-mass galaxies is also shown as gray histograms, normalized to the number of [N II]/Hα-selected AGN and composite galaxies. All values are adopted from StellarMassesG02CFHTLS v24 and StellarMassesGKV v24 tables (Taylor et al. 2011; Bellstedt et al. 2020). Panel (e): the g − r vs. log(M */M ⊙) plot. Here we use similar color scheme as panels (a)–(d). The [N II]/Hα AGNs/composites are among redder and more massive objects in our parent sample, which are similar to He II/Hβ AGNs. The [Fe X] AGNs seem to trace the general trend of our parent sample, while the [Ne V] AGNs are among more massive and bluer objects.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: Galaxies with detectable broad Hα emission from our parent sample with stellar masses M ⋆ ≤ 1010 M ⊙ in the [O III]/Hβ vs. [N II]/Hα diagram (left panel), [O III]/Hβ vs. [S II]/Hα diagram (middle panel), and [O III]/Hβ vs. [O I]/Hα diagram (right panel). As in Figure 3, we use the classification scheme summarized in Kewley et al. (2006). We find 103 galaxies with broad Hα emission, out of which 47 fall in the AGN/composite regions of the [N II]/Hα diagram (orange points). Additionally, six of these are He II-selected AGNs (black squares), one is an [Fe X]-selected AGN (black plus), and one is a [Ne V]-selected AGN (black diamond). The broad Hα objects falling in the star-forming part of the [N II]/Hα diagram (blue points) do not overlap with any of the narrow-line diagnostics used in this work. Only the objects with reliable [S II] and/or [O I] detections are plotted in the middle and right panels. Characteristic error bars are located in the lower right region of each panel. See Section 4.5 for details.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: Chunks of [Fe X] emission-line spectra and the Gaussian emission-line fits for the 56 galaxies with this emission. We plot the single Gaussian models for the [O I]λ6300,6363 lines in blue and the [Fe X]λ6374 line in red. Here the galaxy with CATAID 1787285 is an [N II]/Hα and He II/Hβ AGN, and the object with CATAID 387728 is an [N II]/Hα composite. The [Fe X] lines in our sample have luminosities that span a range of 1038 – 1041 erg s−1, with a median of 1039.6 erg s−1, which can be explained by AGNs or TDEs. See Section 4.3 for details.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: Broad Hα emission. Panels (a)–(b): the distributions of FWHM and log luminosity of the broad Hα components. The [N II]/Hα AGN and composite galaxies are shown as hashed orange histograms, and the star-forming galaxies as blue histograms. See Section 4.5 for details. Panel (c): the virial BH mass distribution for the broad-line AGN candidates. We use Equation (5) in Reines et al. (2013) to estimate these BH masses. See Section 4.5 for details. Note that we do not include the broad-line star-forming objects in our final sample of AGNs.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: Chunks of the He II spectra and the single Gaussian emission-line fits for the 36 He II/Hβ AGN candidates. Here the continuum-subtracted spectrum are shown as black and the individual Gaussian component as orange-red. Ten of these galaxies are [N II]/Hα AGNs, while one is a composite object. See Section 4.2 for details.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: DESI Legacy Imaging Survey SkyViewer grz − band images of dwarf galaxies (M ⋆ ≤ 3 × 109 M ⊙) in our sample with available images (60/70). Red crosses indicate the positions of the spectra and the red dashed circles indicate the sizes of the GAMA spectroscopic fibers (with 2″ diameters).
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: Redshift-corrected spectra and chunks showing [Ne V]λ3426 emission for the three strong [Ne V]-emitting galaxies in this work. Here we plot the best-fitting continuum model and individual Gaussian component as sky blue and orange-red, respectively. These galaxies are also [N II]/Hα AGNs and two of them (CATAIDs 376183 and 694484) are He II/Hβ AGNs. See Section 4.4 for details.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: Redshift-corrected spectra of a selection of [Fe X] AGNs/TDEs overplotted with the continuum model (sky blue). These objects are SF in the [N II]/Hα diagram.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: Redshift-corrected spectra of a selection of He II/Hβ AGNs overplotted with the continuum model (sky blue). These He II/Hβ AGNs are SF in the [N II]/Hα diagram.