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Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Preliminary DPRs for the M31 AGB candidates assuming oxygen- (left) and carbon-rich chemistry (right). The DPRs are estimated by fitting a quadratic to the [3.6]–[4.5] color vs. Log DPR data of the dustiest AGB stars from the SAGE-LMC and SAGE-SMC samples (Groenewegen & Sloan 2018), and applying the relation to our sample. We apply the color–mass-loss relations to all M31 AGB candidates with IRAC 3.6 and 4.5 μm data for the oxygen-rich and carbon-rich case.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption:                         Same as Figure 23, but showing our carbon-rich cluster AGB candidate (green circle). The SED was fit with the carbon-rich J1000-LMC dust-growth radiative-transfer-model grid from Nanni et al. (2019) using the Desk and are shown with assumed distances of 776 kpc. The age of the cluster (Log Age [yr] = 6.9) is likely too young to host an AGB star, and is likely a spatially coincident carbon-rich field AGB star.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: The ratio of x-AGB stars to RGB stars shown in Figure 20 with respect to deprojected radius. The normalized RGB, AGB, and x-AGB sample distributions are shown above in color. The x-AGB fraction peaks around 12 kpc, near the location of recent star formation within the 10 kpc ring.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption:                         Same as Figure 23, but showing the mismatched cluster x-AGB candidate 1765755 (top) and a non-AGB source that we have incorrectly classified (bottom).
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: The spatial distribution of sources classified as x-AGB stars.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Median SEDs of the oxygen-rich, carbon-rich, and x-AGB candidates within the PHAT footprint of M31. We include only sources with IRAC 3.6 μm data and those outside of Brick 1, the region closest to the galaxy center. The data are binned by their absolute IRAC [3.6] magnitude, with a bin size of 0.5 mag, and the number of stars in each bin represented in corresponding color on the right of each figure. We have excluded the MIPS 24 μm mag due to the lower spatial resolution of the observations; we have also removed the medium-band HST data for the x-AGB median SED due to the low number of x-AGB sources with medium-band data. Example model spectra from the COMARCS (Aringer et al. 2009, 2016) code are shown at the top for reference, with two oxygen-rich models at 2600 K (black) and 3300 K (gray), as well as another carbon-rich model at 3400 K, all of which assume no dust. We also show a dusty model created using the DUSTY code (Elitzur & Ivezić 2001).
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: The spatial distribution of the full AGB candidates and distributions of AGB candidate subsets of differing IR magnitude; we omit sources within Bricks 1 and 3, which are significantly affected by crowding. Our most luminous sources are primarily located near the 10 kpc ring, a region of recent star formation. Sources classified in Boyer et al. (2019), which have additional medium-band HST photometry, are included in the AGB catalog. As a result, a higher density of AGB candidates can be seen in these regions in the first panel, shown with white squares in Figure 1.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Spitzer CMDs showing our M31 AGB sample (left), along with the dustiest oxygen-rich (center), and carbon-rich (right) AGB stars found in the MCs (Groenewegen & Sloan 2018). The dust-production rates (DPRs) for the MC samples are shown in color (and size) and were measured using spectral energy distribution (SED) fitting. The threshold at which our Spitzer data are 90% complete (M [4.5] ∼ −9.12 mag) is shown with a dashed line, and the fraction of the dust injected by stars of that chemical subset above this limit is shown as a percentage.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Luminosity functions showing the completeness of our AGB candidates in the IR. The full Spitzer IRAC [3.6] and [4.5] data for M31 (Barmby et al. 2006), the LMC (Meixner et al. 2006), and SMC (Gordon et al. 2011) are included for comparison. While the IR data in the MCs are nearly complete, the M31 IRAC data begin to lose sensitivity around −9 mag, shown in the flattening of the luminosity function. The slope of the fainter AGB sources (dashed line) has been used to estimate the completeness of the data (see Section 3.5.1).
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: The distribution of IRAC [3.6] absolute magnitudes for the carbon-rich samples within M31 and the MCs (Boyer et al. 2011, 2019). Also shown is the luminosity function for the M31 oxygen-rich sample showing that our Spitzer data is able to detect oxygen-rich AGB candidates fainter than our faintest carbon stars.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Histograms of the M31 clusters (blue) and their ages, masses, and metallicities, and the subset of those where we have detected AGB candidates (orange). Also shown are histograms of the fraction of individual sources within clusters, for different cluster properties. The age limit where cluster stars are not expected to have had enough time to evolve to the AGB phase is shown in the shaded region.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Spitzer infrared CMDs of the M31 AGB candidates (black), AGB candidates classified with Spitzer (orange), and cluster AGB candidates (blue). PARSEC isochrones (Marigo et al. 2017) are shown to indicate the end stage of evolution before the onset of AGB mass loss; also shown are error bars calculated using the average photometric uncertainty.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: CMDs of all of the AGB candidates within the PHAT footprint meeting our various criteria. Shown are row 1: an example of the PHAT photometry in Brick 9; row 2: the AGB candidates classified with HST; row 3: the chemically classified subset from Boyer et al. (2019); row 4: the AGB candidates classified with Spitzer; row 5: all criteria combined. The most-yellow regions for each row starting from the HST criteria correspond to densities of around 12, 5, 2, and 12, respectively.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Optical CMDs showing the RHeB candidates and how they are selected. We used the PHAT photometry in Brick 18, where crowding is minimal, to refine our cut. These sources are flagged but included in our AGB catalog.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: The spatial distribution of the AGB candidates identified here (black), outlined by the PHAT footprint. Clusters with known ages and detected AGB candidates are marked with circles (see Section 4), and the medium-band HST footprints where TP-AGB chemical types (carbon- or oxygen-rich) that have been determined by Boyer et al. (2019) are marked with white squares. While our HST data are limited to the PHAT footprint, Spitzer imaging data exists covering the entirety of M31's disk.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Our M31 AGB candidates that were previously classified as oxygen- or carbon-rich (Boyer et al. 2019), with the subsets we have subsequently classified as the dustiest, extreme (x-) AGB candidates (discussed further in Section 4.1). Also shown are the dustiest carbon- (diamonds) and oxygen-rich (squares) sources in the LMC (Groenewegen & Sloan 2018). Extinction vectors with an E(J − K  s ) = 1 mag are shown for oxygen-rich (blue arrow) and carbon-rich (red arrow) dust species, with 60% silicates and 40% AlOx for the oxygen-rich dust and 70% amorphous carbon and 30% SiC dust for the carbon-rich dust.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Our completeness vs. contamination (or rather, sample purity) recovering AGB stars classified with medium-band data (Boyer et al. 2019), using our AGB criteria. Left: the AGB magnitude criteria completeness vs. contamination showing an increasing fraction of the sample having sources with medium-band data but not classified as AGB stars toward fainter magnitudes and below our criteria (shown in gray); our criteria require photometry above the TRGB in the F110W (top axis) or F160W (bottom axis) filters. Shown are the F110W (dotted blue/red lines) and F160W (solid blue/red lines) filter criteria and the fraction of the sample (dashed lines) at our more inclusive magnitude requirement (F110W or F160W) for the completeness and contamination. Right: similar figures showing the AGB color criteria completeness vs. contamination for our color criteria. These figures are limited to sources that also meet our AGB magnitude criteria.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Luminosity functions showing the PHAT catalog, the initial selection of the PHAT catalog (discussed in Section 3.1), the AGB candidates, the chemically classified AGB candidates, and the AGB candidates classified by Spitzer (additional inclusion criteria) for three Brick regions of increasing distance from the galaxy center. For the chemically classified sources in smaller regions within the PHAT footprint, we use all sources ±1 kpc of the deprojected radius value listed below the Brick number in each panel. Also shown are the evolutionary features like the red clump and early AGB bump, and the TRGB (left dashed line). An additional dashed line at 25 mag is plotted for relative comparison.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: A CMD isolating Spitzer sources that are bright and reddened in the IR. These have been included in the AGB catalog irrespective of their HST data (or lack of HST data). PARSEC isochrones (Marigo et al. 2017) are shown to indicate the end stage of evolution before the onset of AGB mass loss and considerable dust production.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: Luminosity functions illustrating the completeness of our M31 data for HST (top) and Spitzer (bottom) in radial arcs across the PHAT footprint. Each radial bin includes all photometry at a specified deprojected radius (r) ±1 kpc, so long as they meet the data quality sharpness and crowding cuts. The TRGB is shown for both filters. Also shown is the median functions of the completeness calculated at 1 kpc intervals, as well as the 68% confidence level around the median calculated by bootstrapping (shown in gray).
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: CMDs showing the Spitzer-GSC data with matches to the Khan (2017) catalog (left), the Khan (2017) catalog with no matches to GSC (center), and binned regions with the fraction of the GSC sources with matches to Khan (2017) shown in color (right). We see no clear biases in the matched-fraction CMD indicating that we are not missing any parts of the IR-CMD in our matching process.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: CMDs showing the chemically classified AGB sample from Boyer et al. (2019) that was used to calibrate the AGB classification criteria (red lines). The oxygen- and carbon-rich stars from Boyer et al. (2019) are shown as green and orange points, respectively. The PHAT photometry for Brick 9 is shown in black, for reference.
Paper: A Census of Thermally Pulsing AGB Stars in the Andromeda Galaxy and a First Estimate of Their Contribution to the Global Dust Budget
Authors: Steven R. Goldman, Martha L. Boyer, Julianne Dalcanton, Iain McDonald, Léo Girardi, Benjamin F. Williams, Sundar Srinivasan, Karl Gordon
Figure caption: An HST-CMD showing the initial cuts to the PHAT catalog. These cuts remove fainter non-AGB sources while still including fainter reddened sources. This cut minimizes spurious matches between the HST and Spitzer data.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Selected chemical abundances with respect to total hydrogen. The results correspond to model basic stage 2, using the medium warm-up timescale. Solid lines indicate gas-phase abundances. Dotted lines of the same color indicate the same species on the dust grains.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Effective diffusion (dashed) and desorption rates (solid) of H2 on an amorphous H2O surface of varying fractional H2 coverage, θ(H2), at a temperature of 10 K. The black lines indicate the unadjusted rates, blue the method used by Garrod & Pauly (2011), and red the new method presented here.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Layer-by-layer ice composition produced during stage 1 (collapse) of the final model setup. All abundances are given as a fraction of the total ice composition (by number) and are local to each layer (rather than cumulative over the total ice thickness formed at a given time). Abundances shown for any particular layer or time in the model (top axis) are those recorded at the moment at which that material is incorporated into the bulk ice. Material in the bulk continues to be processed after its incorporation.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Description as per Figure 5. Results correspond to model bas_stk_loPD_H2_T16_no-bd_3B3_EF stage 1 (collapse). In comparison with the bas_stk_loPD_H2_T16_no-bd model (shown in Figure 5), this setup includes three cycles of the 3-B reaction mechanism, with the 3-BEF process also switched on.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Description as per Figure 2. The results correspond to model bas_stk_loPD_H2_T16_no-bd stage 2, using the medium warm-up timescale. In comparison with the bas_stk_loPD_H2_T16 model (shown in Figure 3), this setup has bulk diffusion switched off for all species except H and H2.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Description as per Figure 5. Results correspond to stage 1 (collapse) of the model final.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Description as per Figure 5. The results correspond to model bas_stk_loPD_H2_T16_no-bd_PDI2 stage 1 (collapse). In comparison with the bas_stk_loPD_H2_T16_no-bd model (shown in Figure 5), this setup includes the PDI2 mechanism in which unreacted photoproduct pairs within the bulk ice are allowed spontaneously to recombine.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Description as per Figure 2. The results correspond to model bas_stk_loPD_H2_T16 stage 2, using the medium warm-up timescale. In comparison with the basic model, this setup includes a uniform sticking coefficient of 1, reduced photodissociation efficiency for solid-phase species, a new treatment for the effect of H2 coverage on surface binding energies, and new gas-phase proton-transfer reactions of large ions with ammonia.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Selected chemical abundances with respect to total hydrogen, for model bas_stk_loPD_H2_T16_no-bd stage 1 (collapse), in which bulk diffusion is switched off for all species except H and H2. Solid lines indicate gas-phase abundances. Dotted lines of the same color indicate the same species on the dust grains. The peak dust temperature is ∼14.7 K. The minimum dust temperature is 8 K.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Description as per Figure 2. Results correspond to model final stage 2, using the fast warm-up timescale.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Description as per Figure 2. Results correspond to model final stage 2, using the medium warm-up timescale.
Paper: Formation of Complex Organic Molecules in Hot Molecular Cores through Nondiffusive Grain-surface and Ice-mantle Chemistry
Authors: Robin T. Garrod, Miwha Jin, Kayla A. Matis, Dylan Jones, Eric R. Willis, Eric Herbst
Figure caption: Net production rates as a function of time; description as per Figure 13. Data correspond to selected nitrogen-bearing molecules in the final model, using the slow warm-up timescale in stage 2.