adsabs/AstroCLIMB huggingface dataset:
Paper: Spectral Templates Optimal for Selecting Galaxies at z > 8 with the JWST
Authors: Rebecca L. Larson, Taylor A. Hutchison, Micaela Bagley, Steven L. Finkelstein, L. Y. Aaron Yung, Rachel S. Somerville, Michaela Hirschmann, Gabriel Brammer, Benne W. Holwerda, Casey Papovich, Alexa M. Morales, Stephen M. Wilkins
Figure caption: Plots illustrating the details of the selection criteria cuts we made to select for high-redshift galaxies and the impact each cut has on our final sample. In each figure, we plot the real z > 8 sources in our sample in blue and the contaminating z < 5 galaxies in red. Prior to the cuts shown here, we required an S/N > 5 in both F200W and F277W and an ∫P(z > 7) > 0.85 (see Section 7) which left us with a sample of 4902 potential high-redshift (z > 8) galaxies. We then make a cut in χ 2 of the EAZY fit (left) which removes 576 sources, 460 of which were contaminating low-redshift galaxies. In Section 7.1, we discuss the need for additional selection criteria that will remove contaminating low-redshift interlopers from our sample and that the above two color cuts: F150W − F444W (center) and F150W − F200W (right) were the two that most distinguished between these two sets of galaxies remaining in our sample. After requiring an F150W − F444W color < 0.3 and F150W − F200W < 0.2, we are able to remove an additional 1410 sources, 1394 of which are contaminants, while only losing 16 real z > 8 galaxies from the sample. We show the remaining 2670 sources in our sample and their distribution in true redshift and F200W magnitude in Figure 7, showing that a majority of the contaminants are at m > 28.
Paper: Spectral Templates Optimal for Selecting Galaxies at z > 8 with the JWST
Authors: Rebecca L. Larson, Taylor A. Hutchison, Micaela Bagley, Steven L. Finkelstein, L. Y. Aaron Yung, Rachel S. Somerville, Michaela Hirschmann, Gabriel Brammer, Benne W. Holwerda, Casey Papovich, Alexa M. Morales, Stephen M. Wilkins
Figure caption: Our final sample of high-redshift galaxies after making cuts based upon the five selections detailed in Section 7. Here we plot these sources by their input redshift from the SAM vs. the F200W perturbed magnitude with corresponding histograms for each axis. Our final sample includes 2670 sources, 1294 of which are contaminating z < 5 galaxies while 897 are actual z > 8 sources. The horizontal line shows that the sample is dominated by low-z contaminants at m ≳ 28 but brighter than m ∼ 27. All of our selected sources are high-redshift galaxies. This shows that, with the colors from sources in this simulated catalog, near our survey detection limits, we struggle with distinguishing these high-redshift sources from low-redshift interlopers, though we expect the true contamination rates in observations to be lower than those predicted here (Section 7.3). Figure 8 shows details about our contamination and completeness fractions.
Paper: Spectral Templates Optimal for Selecting Galaxies at z > 8 with the JWST
Authors: Rebecca L. Larson, Taylor A. Hutchison, Micaela Bagley, Steven L. Finkelstein, L. Y. Aaron Yung, Rachel S. Somerville, Michaela Hirschmann, Gabriel Brammer, Benne W. Holwerda, Casey Papovich, Alexa M. Morales, Stephen M. Wilkins
Figure caption: Completeness and contamination fractions as a function of magnitude in several distinct redshift bins. As illustrated in Figure 7, we suffer from high contamination rates at the faint end of our sample (m > 27.5) at all redshifts. It is also notable that the redshift range at which we recover the highest fraction of real z > 8 galaxies is above z = 9.5 where the Lyα break falls within the JWST filters, providing the SED-fitting process the clearest high-redshift feature. Overall, we maintain a high recovery (completeness) fraction for our galaxies, where we recover a total of 897 of 1325 real z > 8 sources in the SAM. The ones being missed by our selection criteria are predominantly at the faint end, close to our detection limits, and where we are most dominated by contamination.
Paper: Spectral Templates Optimal for Selecting Galaxies at z > 8 with the JWST
Authors: Rebecca L. Larson, Taylor A. Hutchison, Micaela Bagley, Steven L. Finkelstein, L. Y. Aaron Yung, Rachel S. Somerville, Michaela Hirschmann, Gabriel Brammer, Benne W. Holwerda, Casey Papovich, Alexa M. Morales, Stephen M. Wilkins
Figure caption: Plots illustrating the accuracy of our recovered redshifts from EAZY vs. input redshifts for our mock CEERS observations of the SAM galaxies. We show the full z = 0–10 set of 913,288 galaxies in the SAM (top), and a zoom-in on the z = 8–10 range of particular interest to JWST studies (bottom). Left: the median Δz as a function of redshift, separated in bins of F200W magnitude. Center: the standard deviation (NMAD) of our Δz in corresponding magnitude bins. Right: the fraction of outliers in our fits where we define outliers as those with a Δz > 2 binned in magnitude. For each of these parameters, we note that the faint galaxies (m > 27.5) are the sources with the least accurate recovered redshifts, which is not unexpected as constraints on their colors are the poorest.
Paper: On the “Loose” Constraint from IceCube Neutrino Nondetection of GRB 230307A
Authors: Xin-Ying Song
Figure caption: Panels (a) and (b) are allowed and excluded ranges of Γ, ξ N, and ζ  n  in np decoupling mechanism. The blank around lower Γ and higher ξ N is the np coupling region where Γ < Γ np . The red dashed line denotes that of GRB 221009A. The gray vertical lines denote the Γ = 400 for (a) and ζ  n  = 2.3 and 5.7 for (b). (c) The allowed and excluded ranges of ξ N in the np collision mechanism. The vertical line denotes τ  np  = 1.
Paper: On the “Loose” Constraint from IceCube Neutrino Nondetection of GRB 230307A
Authors: Xin-Ying Song
Figure caption: (a) The light curves (logarithm scale) of GBM na detector and α, E p values, with a subplot (b) for the first 1 s. Red circles and blue triangles denote α values from the fit results with BAND and CPL functions (the same below), respectively. Green diamonds denote the E p values from the fit results. The subplot shows α and E p values of the first 1 s. (c)–(h) Time-resolved spectra with modeling with multi-blackbody (mBB) or mBB+PL functions.
Paper: On the “Loose” Constraint from IceCube Neutrino Nondetection of GRB 230307A
Authors: Xin-Ying Song
Figure caption: (a) and (b) the nonthermal neutrino spectra with Γ = 400 for GRB 230307A and GRB 221009A of different emission mechanisms. For GRB 221009A, f p is calculated to be about 0.3, 0.5, and 0.3 for PH, ICMART, and IS models, respectively; for GRB 230307A, f p is calculated to be about 0.3, 0.7, and 0.5 for PH, ICMART, and IS models, respectively. Panels (c) and (d) are allowed ranges of Γ, R  d , and ξ CR. The solid red line denotes the UL at 90% CL of GRB 230307A. The blue dotted line denotes 1 order of magnitude lower than UL=1 GeV cm−2. The allowed ranges are below the corresponding lines, while the excluded ranges are above them, the same below.
Paper: Interplanetary Signatures during the 1972 Early August Solar Storms
Authors: Consuelo Cid, Elena Saiz, Manuel Flores-Soriano, Delores J. Knipp
Figure caption: Explorer 41 (IMP 5) magnetic field measurements in solar-ecliptic coordinates, digitized from Figure 15 from Smith (1976), and Prognoz 2 plasma measurements during 1972 August 2–17, digitized from Figure 1 from d’Uston (1982).
Paper: Interplanetary Signatures during the 1972 Early August Solar Storms
Authors: Consuelo Cid, Elena Saiz, Manuel Flores-Soriano, Delores J. Knipp
Figure caption: Pioneer 10 IP magnetic field and solar wind plasma measurements during 1972 August 5–16. Solid black lines correspond to 1 minute magnetic field data (strength and RTN components) and hourly plasma data (proton speed, temperature, and density) downloaded from CDAWeb.                    Plasma data digitized from Figure 1 of Mihalov et al. (1973) are overplotted using the blue dot symbol. Red line in sixth panel corresponds to the expected temperature (Richardson & Cane 1995). The IP shocks of Table 1 appear as black triangles at the bottom of every panel and are labeled in the bottom panel. Colored areas indicate the ICME intervals and the gray shadowed area indicates a high-speed stream region.
Paper: Interplanetary Signatures during the 1972 Early August Solar Storms
Authors: Consuelo Cid, Elena Saiz, Manuel Flores-Soriano, Delores J. Knipp
Figure caption: The events observed at different heliocentric distance from the Sun to Pioneer 10 orbit at 2.2 au. Dots correspond to the events in Table 1, and solid lines represent their association according to Dryer et al. (1975). Dashed lines indicate the radial propagation along the Sun-Pioneers line. Colored areas correspond to ICME intervals, gray areas correspond to high-speed streams, and stars indicate ICME–ICME interaction. See Section 2 for details.
Paper: Interplanetary Signatures during the 1972 Early August Solar Storms
Authors: Consuelo Cid, Elena Saiz, Manuel Flores-Soriano, Delores J. Knipp
Figure caption: The events observed at different heliocentric distance from the Sun to Pioneer 10 orbit at 2.2 au. Dots correspond to the events in Table 1, and solid lines represent their association according to Dryer et al. (1975).
Paper: Interplanetary Signatures during the 1972 Early August Solar Storms
Authors: Consuelo Cid, Elena Saiz, Manuel Flores-Soriano, Delores J. Knipp
Figure caption: Pioneer 9 IP magnetic field and plasma measurements during 1972 August 2–17 digitized from Figures 1 and 2 of Mihalov et al. (1973).
Paper: Interplanetary Signatures during the 1972 Early August Solar Storms
Authors: Consuelo Cid, Elena Saiz, Manuel Flores-Soriano, Delores J. Knipp
Figure caption: Position of spacecraft in 1972 August in the ecliptic plane.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: CMD of GO stars. CMD of the stars in the GO data set. The black dots show the stars with fixed log(g) in our SPEXXY fit while the orange points have free log(g), and the purple are the horizontal-branch stars, which are disregarded in the current analysis. The yellow points indicate the position of the isochrone used to infer the log(g).
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Error analysis correction. Top panels: the x-axis is the S/N, and the y-axis is the σ 2 of the Δ[M/H] for the GO data on the left and the GTO data on the right. The red line is the best-fitting first-order polynomial, the black dots are our data values, and the light red shaded area is the region below an S/N of 10, which we exclude from the analysis. Bottom panels: the x-axis is the S/N and the maximum percentage of counts one star has in each bin. The red dashed line shows the maximum number of measurements each star can have, which is clearly always below 10% of the total number of measurements in each bin, making sure the statistics in each bin are not the result of only one star.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Image of ω Cen and footprint of the MUSE pointings. On the left is a gray-scale image created from the combined GO and GTO MUSE WFM data. Overlaid blue colored squares indicate the GO AO pointings, red squares the WFM GTO data, while the region without squares is where the non-AO GO WFM pointings lie. On the right is the footprint of the individual pointings showing the overlap of the data. At the center of the right-hand figure, the NFM data are within the yellow region at the center of the image, indicated with a red cross.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: All extracted GO stars. The figure shows the positions of all extracted GO stars using the Anderson & van der Marel (2010) photometric catalog. The red cross indicates the center, while the holes at the top and at the center are later filled with the GTO stars. Some edges are cut off because the Hubble Space Telescope footprint does not perfectly cover the MUSE footprint. The overlap regions are denser, since more stars are observed due to the fact that there are two or more exposures. The variation in the number of stars seen in different fields is due to varying observing conditions that impact our completeness.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Example spectra. (a)–(d) Spectra of stars at different stages of evolution plotted in black, with best-fitting SPEXXY models in red. The light red shaded areas are the excluded/masked regions during the fit. Note that the RGB star (d) is observed with AO, and the NaD line is blocked. The bottom panels show the data model residuals in blue. We note that the deep broad absorption features at 6800 and 7600 Å are telluric features that are fit by SPEXXY along with the stellar properties. The best-fitting parameters for S/N, [M/H], vlos, Teff, and the log(g) value are given on top of each spectrum.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: GO Completeness plots. On the left is the overall GO completeness (the combined completeness for all 87 GO pointings) for different S/N cuts, from left to right, the S/N is decreasing. The dashed line indicates 50% completeness, and the dotted line is 18.86 mag in F625W. The right plot shows for an S/N > 10 the individual completeness for three pointings at different radii from the center.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Membership probabilities using radius and velocity for an S/N>10. The stars’ radial distances to the cluster center in arcminutes are plotted against their line-of-sight velocities. The points are color coded according to their membership probability, yellow being 1.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Error analysis CDF. The cumulative distribution of the Δ[M/H] in black for S/N >10 for the GO data and in red the distribution if it was a normal distribution. The dashed black line is the distribution after the error correction.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Image of ω Cen. A three-color RGB image of ω Cen created from MUSE WFM data using synthetic SDSS i, r, and g filters. The image displays the coverage of all WFM data (both GTO and GO). The red cross indicates the center of the cluster.
Paper: Linking the Metallicity Enrichment History to the Star Formation History: An SFH-regulated Chemical Evolution Model and Its Implications for the Gas Cycling Process
Authors: Jun Yin, Shiyin Shen, Lei Hao
Figure caption: Time evolution of the dSph galaxies Cetus (left column) and Tucana (right column). The SFHs measured by the CMD fitting method are shown in cyan (Skillman et al. 2014) in panels (a.1) and (a.2), and the black solid lines are used as the input SFHs in our model. The time evolution of the gas surface density is shown in panels (b.1) and (b.2). In panels (c.1) and (c.2), the black solid lines represent the net gas flow rate. The gas inflow and outflow histories are shown in panels (d) and (e), and the MEHs predicted by our model (black lines) compared with those measured by Skillman et al. (2014; cyan) and D. Weisz (2023, private communication; yellow triangles) are shown in panel (f). The black dotted, dashed, solid, and dashed–dotted lines indicate the η = 0.0, 0.5, 1.0, and 2.0 cases, respectively. In the case of Tucana, all of the evolution histories are shown as gray after t ∼ 6 Gyr. We also overplotted the evolution histories predicted by the CB (blue dotted lines) and LKB (red dashed–dotted lines) models as a comparison (see Section 5.1 for more details).
Paper: Linking the Metallicity Enrichment History to the Star Formation History: An SFH-regulated Chemical Evolution Model and Its Implications for the Gas Cycling Process
Authors: Jun Yin, Shiyin Shen, Lei Hao
Figure caption: Metallicity–gas fraction (Z–μ) relation. The colored vertical bars show the observation data of six LCID galaxies; the gas fractions of LCID galaxies are calculated from the total gas and stellar mass listed in Table 1, and the metallicity represents the range from the observed metallicity of the region where the CMD was measured to the entire galaxy. The colored lines represent the predictions of our SFH-regulated model for each LCID galaxy with the same color as its observed data. The dotted, dashed, dashed–dotted, and solid lines represent cosmic time ranges of [0, 3], [3, 7], [7, 10], and [10, 13.5] Gyr, respectively. The black dotted, dashed–dotted, and dashed lines represent the evolution track of the CB, LKB (Zhu et al. 2017), and B18) models, respectively.
Paper: Linking the Metallicity Enrichment History to the Star Formation History: An SFH-regulated Chemical Evolution Model and Its Implications for the Gas Cycling Process
Authors: Jun Yin, Shiyin Shen, Lei Hao
Figure caption: Time evolution of dIrr galaxies IC 1613 and Leo A. Similar to Figure 2, this figure shows the evolution of the SFR, the gas surface density, the net gas flow rate, the gas inflow and outflow rates, and the MEH from top to bottom.
Paper: Linking the Metallicity Enrichment History to the Star Formation History: An SFH-regulated Chemical Evolution Model and Its Implications for the Gas Cycling Process
Authors: Jun Yin, Shiyin Shen, Lei Hao
Figure caption: Observed SFHs and MEHs of six LCID galaxies. Two dSphs, Cetus and Tucana, are shown with red lines (Monelli et al. 2010a, 2010b); two dTrans, LGS 3 and Phoenix, are shown with blue lines (Hidalgo et al. 2009, 2011); and two dIrrs, IC 1613 and Leo A, are shown with black lines (Cole et al. 2007; Skillman et al. 2014). The upper panel shows the evolution histories of SFR surface density, whereas the lower panel shows the MEHs.
Paper: Linking the Metallicity Enrichment History to the Star Formation History: An SFH-regulated Chemical Evolution Model and Its Implications for the Gas Cycling Process
Authors: Jun Yin, Shiyin Shen, Lei Hao
Figure caption: Time evolution of dTran galaxies LGS 3 and Phoenix. Similar to Figure 2, this figure shows the evolution of the SFR, the gas surface density, the net gas flow rate, the gas inflow and outflow rates, and the MEH from top to bottom.
Paper: Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies
Authors: Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham
Figure caption: Upper panel: DM host minor-axis orientation plots of m12f, m12i, m12m, and m12w as a function of radius at z = 0. The distance ranges for Gaia (for MSTO), ground-based M-giant asteroseismology, and LSST are shown with the different line styles. Lower panel: DM triaxiality plots of m12f, m12i, m12m, and m12w as a function of radius at a redshift of z = 0. Triaxiality is determined by the convergent ellipsoid at each radius. The horizontal lines demarcate the transitions between oblate (T < 1/3), triaxial (1/3 < T < 2/3), and prolate (T > 2/3) shape classifications. This plot is available as a function of time in Figure 9.
Paper: Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies
Authors: Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham
Figure caption: The misalignment angle of the DM halo minor axis relative to the stellar component over time at different scale lengths. The yellow solid line is the orientation of the DM halo at the edge of the stellar component of the galaxy (R *,90), the green dashed line is the orientation outside the galaxy but well within the DM halo (5 × R *,90), and the blue dashed–dotted line is the global orientation of the DM halo at R 200m. Orientations at each snapshot are calculated with respect to the galaxy vector at that particular snapshot. The vertical black line indicates when the LMC analog reaches pericenter for the particular galaxy and the red line indicates when the thin disk of the galaxy begins to form.
Paper: Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies
Authors: Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham
Figure caption: Halo orientations relative to the stellar disk for different simulations at z = 0. Each galaxy begins with identical initial conditions, with the exception of how the DM interacts within the system. The gray line represents the orientation of the halo with CDM and baryons (see Figure 3), and the light blue (dark blue) lines correspond to DMO (SIDM) halo orientations. Additionally, we plot distance ranges for Gaia (MSTO), M-giant asteroseismology, and LSST. The DMO pseudo-stellar disk axis is defined to be the angular momentum of the DM particles within 10 kpc.