adsabs/AstroCLIMB huggingface dataset:
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Demonstration of the exclusion of BHeB stars from CMD modeling, using Leo A as an example. Left panel: identification of HeB stars (purple circles) in the (F275W − F475W, F475W) CMD based on isochrones adapted for Leo A, as shown in Figure 4. Crosses represent spectroscopically confirmed Be stars from M. Gull et al. (2022), which are included in our final CMDs. However, they fall within the excluded CMD regions, ensuring no impact on our SFH measurements. Notably, these confirmed Be stars are indistinguishable from BHeB stars based solely on their optical photometry. Middle and right panels: the identified HeB stars are roughly divided into blue HeB (BHeB) and red HeB (RHeB) stars based on their optical colors. BHeB stars, which are excluded from the stellar catalogs for the SFH fits, are marked with blue circles, while retained RHeB stars are marked with red circles in both the optical and UV CMDs used for the UVopt case. Black dashed lines indicate the regions of the CMDs that are excluded from the SFH fitting calculations, ensuring that MATCH does not misinterpret the absence of BHeB stars during the CMD modeling process.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Each row displays an example realization of synthetic UV and optical CMDs for a Leo A–like galaxy, with exaggerated recent SF activity, modeled under different dust extinction scenarios: (dAV, d﹩{A}_{{V}_{{\rm{y}}}}﹩) = (0.1, 0.2), (0.2, 0.1), (0.0, 0.5), and (0.2, 0.7) from top to bottom. The left two panels display UV CMDs color-coded by stellar age and total dust, and the right two panels show optical CMDs with the same color coding. This layout highlights the impact of dust on the appearance of UV and optical CMDs, as well as the effect of stochastic sampling in the high end of the IMF. Note that these CMDs are shown prior to applying photometric uncertainties as well as completeness limits to maintain clarity in presenting the impacts of stellar age and total dust on the locations of stars in the CMDs.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Differential SFHs for the 10 galaxies over the past 1 Gyr, with error bars indicating 1σ random uncertainties. For each galaxy, the gray dashed lines represent the average SFR over the past 1 Gyr. The SFHs exhibit stochastic fluctuations, with all 10 galaxies showing multiple age bins where the SFRs exceed their 〈SFR〉1 Gyr by a factor of a few to several. This underscores the episodic nature of SF in these metal-poor dwarf galaxies.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Reversed cumulative SFHs of the past 1 Gyr for the 10 galaxies, with a shaded envelope indicating 1σ random uncertainties. To better visualize the fraction of stellar mass formed in recent time bins, we reverse the cumulative calculation backward in time, setting the cumulative stellar mass fraction to 0 at the present and setting it to 1 at 1 Gyr ago, and display the y-axis on a logarithmic scale. For each galaxy, the gray dashed lines represent a constant SFH scenario, illustrating the average SFR over the past 1 Gyr and appearing as a straight line. The abrupt drop below log10(t/[yr]) = 6.3 arises from the challenge of representing a value of 0 on a logarithmic scale.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Same as Figure 8, but for the constant SFH with (dAV, d﹩{A}_{{V}_{{\rm{y}}}}﹩) = (0.0, 0.5) as an input, where the SFR is set to 0.01 M⊙ yr−1 over the past 1 Gyr and 0 at earlier times.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Input SFH and chemical enrichment history used to simulate UV and optical CMDs. The input SFH is based on a modified version of Leo A’s best-fit SFH and chemical enrichment history from the UVopt solution (Section 4), with a constant SFR of 0.01 M⊙ yr−1 over the past 10 Myr to enhance the upper MS, facilitating a clearer assessment of the impact of UV inclusion.
Paper: Solar, Dust, and Tidal Effects on Martian Dayside Exospheric Temperature: An Empirical Model Based on a Decadal MAVEN/IUVS Data Set
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a) Color coded: latitude coverage of the IUVS observations. Magenta: SMD in astronomical unit (au). (b) Color coded: Martian dayside Texo estimated from IUVS Lyα limb scans. Red: Martian dayside Texo calculated by using the empirical model of J. M. Forbes et al. (2008). The Texo estimates that are marked with rectangles “A” and “B” will be further examined in Figure 3. (c) Color coded: CDOD associated with the times and geographic locations of the IUVS observations. Orange: solar Lyα flux measured by EUVM. Blue dashed: CDOD = 0.3. The color bar in panel (b) applies to all panels (a), (b), and (c), with the data in each panel color coded according to the local time of the observations. MY: Martian year.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Each row compares the UVopt and Opt-only SFHs for Leo A, DDO 210, SagDIG, UGC 8091, and UGC 8508. Left panels: differences between the UVopt and Opt-only differential SFHs over the past 1 Gyr. The error bars represent the combined uncertainties from the UVopt and Opt-only SFHs, computed by adding their individual uncertainties in quadrature. Generally, the UVopt SFHs yield lower SFRs (i.e., negative values in the plot) and reduced uncertainties compared to the canonical Opt-only SFHs in most recent time bins. Middle panels: cumulative SFHs for both cases, shown with the 68% confidence interval. The specific lookback time at which the two SFHs begin to diverge varies across galaxies. However, despite these variations in divergence timing, the overall impact on the total stellar mass formed remains small. Specifically, the discrepancies in the SFH affect at most the formation of the last few percent to 10% of the total stellar mass. Right panels: average SFRs as a function of τ for both cases. The calculation of average SFRs for each τ and their associated uncertainties is described at the beginning of Section 4.2. Notably, the UVopt SFHs show smaller uncertainties compared to the canonical Opt-only SFHs, particularly in age bins younger than 100 Myr, a trend also observed in the simulated SFHs (Section 3.3).
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Top panel: comparison of the CMD-based 〈SFR〉10 Myr with the Hα-based SFRs from L09 (circles) and K13 (crosses). The dashed line represents the one-to-one relationship. We also present the comparison against 〈SFR〉10 Myr from the Opt-only SFHs (gray open symbols). Bottom panel: the ratio of the CMD-based 〈SFR〉10 Myr to the Hα-based SFRs is plotted against the Hα-based SFRs, with the dashed line indicating a ratio of unity. The discrepancy between the Hα-based SFRs and the CMD-based 〈SFR〉10 Myr increases at lower SFRs. This trend is expected, as converting a global Hα to an SFR becomes unreliable in this low-SFR regime, where the assumptions of a fully populated IMF and a constant SFR over the most recent 10 Myr break down (e.g., R. C. J. Kennicutt et al. 2008). The dotted line represents a ratio of 10, an estimated upper limit on the underestimation of SFRHα assuming the observed Hα luminosity predominantly originates from a single starburst within the past 1 Myr.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Ratio of 〈SFR〉Opt-only to 〈SFR〉UVopt at the τ = 50 Myr against the total dust extinction (left panel) and differential dust extinction (middle panel) derived from the UVopt solutions, as well as the difference in the total dust extinction between the UVopt and Opt-only solutions (right panel). These three cases are the only ones that show statistically significant correlations (p-value < 0.05) among the various properties investigated, including dust content, Hα- and FUV-based SFRs, and oxygen abundance over 10 Myr < τ < 1 Gyr. The Pearson correlation coefficient (r) with its uncertainty and the p-value are noted at the top of each panel. The common τ = 50 Myr across all three correlations aligns with the 40 Myr threshold in MATCH, where d﹩{A}_{{V}_{{\rm{y}}}}﹩ is fully applied to younger stars and decreases linearly to zero by 100 Myr. This suggests that differences in dust extinction treatment between the canonical Opt-only and UVopt cases primarily drive the SFH discrepancies in recent time bins.
Paper: Solar, Dust, and Tidal Effects on Martian Dayside Exospheric Temperature: An Empirical Model Based on a Decadal MAVEN/IUVS Data Set
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a) Variation of the Texo estimates with solar Lyα flux, color coded by the SMD. Red: a linear fit to the Texo estimates, with a slope of 45 K mW−1 m2. (b) Local time variation of the Texo estimates. Black line and gray shaded area: mean temperature and standard deviation that are obtained by averaging all individual measurements within latitudes of 60°S–60°N. Circles and vertical bars: mean temperature and standard deviation that are averaged under (red) high solar Lyα flux of 3.4–3.6 mW m−2 and (blue) low solar Lyα flux of 2.2–2.4 mW m−2, respectively. The bin size is 1 hr.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Same as Figure 16, but for UGC 9240, NGC 4163, NGC 3741, DDO6, and UGCA 292.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: CMD-based average SFRs from the UVopt SFH across various timescales (10 Myr, 20 Myr, 30 Myr, 40 Myr, 50 Myr, 70 Myr, 100 Myr, 160 Myr, 200 Myr, 300 Myr, 500 Myr, 700 Myr, and 1 Gyr) are illustrated. We also plot the integrated flux-based SFRs for each galaxy, adopted from the literature. Magenta lines indicate dust-corrected Hα-based SFRs, whereas purple lines indicate dust-corrected FUV-based SFRs. The solid lines are from J. C. Lee et al. (2009), and the dashed lines are from I. D. Karachentsev et al. (2013). These literature SFRs are listed in Table 2 along with those computed from our CMD-based SFHs.
Paper: The Local Ultraviolet to Infrared Treasury. II. Refining Star Formation Histories of 10 Metal-poor Dwarf Galaxies with Simultaneous UV-optical Two-CMD Fitting
Authors: Yumi Choi, Karoline M. Gilbert, Benjamin F. Williams, Daniel R. Weisz, Evan D. Skillman, Julianne J. Dalcanton, Kristen B. W. McQuinn, Andrew E. Dolphin, Giada Pastorelli, Martha L. Boyer, Karl D. Gordon, Léo Girardi, Maude Gull
Figure caption: Comparison of the CMD-based 〈SFR〉100 Myr and the FUV-based SFRs. Symbols and lines are the same as in Figure 14. In most galaxies, the CMD-based 〈SFR〉100 Myr values from the UVopt SFHs are lower than the FUV-based SFRs, whereas the 〈SFR〉100 Myr values from the Opt-only SFHs are higher. Despite the opposing trends between the two SFH cases, the overall deviations are moderate, with ratios ranging from approximately 0.5–2.
Paper: Solar, Dust, and Tidal Effects on Martian Dayside Exospheric Temperature: An Empirical Model Based on a Decadal MAVEN/IUVS Data Set
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a) Longitudinal structure of the Texo estimates near aphelion (Ls = 85°–100°) in MY 34 under relatively low solar Lyα flux between 2.24 and 2.43 mW m−2, local time from 10 to 12 hr, and latitudes between 40°S and 18°N. Black circles: mean temperature, averaged over 10° longitudes. Vertical bars: standard deviations. Red line: a harmonic fit. (b) Same as (a), except for near perihelion (Ls = 336°–343°) in MY 36 under relatively high solar Lyα flux between 3.31 and 3.62 mW m−2, local time from 13 to 16 hr, and latitudes between 75°S and 36°S. LT: local time. Lat: latitude. Ls: solar longitude.
Paper: Solar, Dust, and Tidal Effects on Martian Dayside Exospheric Temperature: An Empirical Model Based on a Decadal MAVEN/IUVS Data Set
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a) Gray: Texo estimates from the IUVS Lyα observations, same as those shown in Figure 1(b). Red: Texo values calculated by using the complete form of our empirical model, with solar, seasonal, tidal, and dust effects included. (b)–(c) Zoom-in views of the two periods of time that are marked with rectangles in (a). Red and gray: same as those shown in (a). Blue: modeled Texo without considering the dust effect, which is calculated by using our empirical model without the F3 term in Equation (2) (i.e., dust-free model). (d) Same as Figure 3(b), except that the individual Texo values that are averaged to obtain the mean and standard deviations are calculated by using the complete form of our empirical model.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: The structure of the local interstellar medium (LISM) is shown in the x–y plane of the Galaxy (where +x is directed toward (l, b) = (0°, 0°) and +y is directed toward (90°,0°). The green regions show a cross section of the Local Hot Bubble (LHB) wall as provided by T. J. O’Neill et al. (2024), with the inner, peak, and outer surfaces indicated. The outlines of the LIC and G-Cloud (as found by S. Redfield & J. L. Linsky 2008) are shown in red and light brown, respectively, magnified by 20×. To indicate the orientation of the solar system and for comparison with Figure 1, the trajectories of the five escaping spacecraft and the orbit of Neptune are projected onto the x–y plane, magnified by 100,000×. The locations of 54 UV-bright stars are projected onto the x–y plane, with blue for O and B stars inside the outer wall of the LHB and purple for three nearby EUV-bright white dwarfs (G191B2B, Feige 24, and HZ43).
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: The trajectories of the five spacecraft currently leaving the solar system: Pioneer 10 and 11 (orange and light green, respectively), Voyager 1 and 2 (gray and green, respectively), and New Horizons (NH, red) are shown projected onto the plane of the ecliptic, along with several planet orbits (black) and the direction of the flow of interstellar hydrogen atoms (purple arrows). The locations where great-circle scans of interplanetary medium (IPM) Lyα were made with the NH Alice UV spectrograph are indicated (red), including the all-sky Lyα map described here, which was executed during 2023 September 2–11 at a distance from the Sun of 56.9 au.
Paper: Solar, Dust, and Tidal Effects on Martian Dayside Exospheric Temperature: An Empirical Model Based on a Decadal MAVEN/IUVS Data Set
Authors: Zhen Xu, Jianqi Qin
Figure caption: (a) Gray: exobase altitude (hexo) derived from the NGIMS measurements based on Equation (7). Orange: the Texo estimates that are averaged over each MAVEN orbit. (b) Black: exobase altitude vs. Texo. Red: a linear fit to the observations, with hexo = 0.32Texo + 147.58 km. (c) Black: H thermal escape rate, ϕH, vs. Texo. Red: a quadratic fit, with ﹩{\mathrm{log}}_{10}{\phi }_{{\rm{H}}}=-1.08\times 1{0}^{-4}{T}_{{\rm{exo}}}^{2}+0.06{T}_{{\rm{exo}}}-0.29﹩ cm−2 s−1.
Paper: Solar, Dust, and Tidal Effects on Martian Dayside Exospheric Temperature: An Empirical Model Based on a Decadal MAVEN/IUVS Data Set
Authors: Zhen Xu, Jianqi Qin
Figure caption: Variations of Texo calculated with our empirical model. (a) Seasonal variation at lat = 5°N, lon = 0°, and LT = 12 hr under different solar and dust conditions. (b) Latitudinal variation at lon = 10° and LT = 10 hr in the northern summer (Ls = 60°) and southern summer (Ls = 280°) under different solar activity. Moderate solar: F10.7A = 65 sfu. Low solar: F10.7A = 25 sfu. Dusty: τ = 0.35. Low dust: τ = 0.1.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: The structure of the local interstellar medium (LISM) is shown in the y–z plane of the Galaxy (where +y is directed toward (l, b) = (90°, 0°) and +z is directed toward (0°, 90°). The rest of the figure is as in Figure 2, except that the outlines of the LIC and G-Cloud are not shown.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: The structure of the local interstellar medium (LISM) is shown in the x–z plane of the Galaxy (where +x is directed toward (l, b) = (0°, 0°) and +z is directed toward (0°, 90°). The rest of the figure is as in Figure 2, except that the outlines of the LIC and G-Cloud are not shown.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: All-sky New Horizons Alice Lyα maps derived from analog count rates (as processed in the manner described in Figure 5) and converted to brightness using the sensitivity value of 3.67 counts s−1 R−1 (1 R = 106 photons cm−2 s−1 (4πsr)−1) that is derived in Appendix A. The upper map is in ecliptic coordinates centered on the anti-Sun direction, and the lower map is in Galactic coordinates, centered on (l, b) = (0°, 0°). Both Mollweide projection maps show Alice brightnesses (except for the 30° swath containing the Sun, which shows a hot model estimate of the backscattered solar Lyα plus a 50 R value meant to represent the Galactic Lyα signal). The ∼90,000 stars in the M. A. Velez et al. (2024) catalog are overlaid as black dots, where the size of the dot is proportional to the logarithm of the expected Alice count rate from each star. The map in Galactic coordinates indicates the outlines of four of the important LISM clouds (“LIC,” in red; “Aql,” in green; “Blue,” in blue; and “G,” in tan), as described in S. Redfield & J. L. Linsky (2008). The locations of 14 fast-moving stars from J. M. Shull & S. R. Kulkarni (2023), listed here in Table 2, are indicated by light blue dots, with lines extending to their expected locations in 104 yr. Both maps also include directions for the poles of the alternate projection map, the upstream and downstream directions of the flow of interstellar H I through the solar system, and the Sun. The Galactic All-sky New Horizons Alice Lyα map shown in panel (b) of this figure is available as data behind figure in FITS format. These data can also be used to obtain the results shown in Figure 7(b).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)