adsabs/AstroCLIMB huggingface dataset:
Paper: Orbital Characterization of Superbolides Observed from Space: Dynamical Association with Near-Earth Objects, Meteoroid Streams, and Identification of Hyperbolic Meteoroids
Authors: Eloy Peña-Asensio, Josep M. Trigo-Rodríguez, Albert Rimola
Figure caption: Histogram of the principal parameters and the calculated orbits of the 255 CNEOS studied events in this work. The y-axis is arbitrarily scaled.
Paper: Orbital Characterization of Superbolides Observed from Space: Dynamical Association with Near-Earth Objects, Meteoroid Streams, and Identification of Hyperbolic Meteoroids
Authors: Eloy Peña-Asensio, Josep M. Trigo-Rodríguez, Albert Rimola
Figure caption: Dissimilarity criteria of 2020-03-04 20:25:59, 2014-11-26 23:16:51, 2005-04-19 07:37:47, and 2017-05-24 07:03:03 events in relation to their respective associations over a backward integration of 10,000 years. A dashed horizontal line shows the cut-off for each criterion.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Level curves of the adiabatic invariant S (left panel) and time histories of the angles σ and ω for the trajectory propagated under the full N-body model (right panel) for 2018 VO137, which is currently inside 2:5 resonance with Neptune. The parameters for this TNO are provided in Table 2. In the left panel, the trajectory propagated in the full N-body model is shown by a blue line and the one propagated in the semi-secular model by a green line. The critical curve is marked by red dots (the region above the curve corresponds to libration and that below to circulation). Evidently, the trajectory of 2018 VO137 intersects the critical curve twice in a ZLK period, showing that in the long-term evolution the resonant angle σ switches between libration and circulation periodically. In the considered time interval, 2018 VO137 is currently located inside the ZLK island centered at ω = 90°.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Level curves of the adiabatic invariant, S, plotted in the space ﹩(\omega ,\widetilde{e})﹩ (left panel), and three representative examples with S = 0.001555, plotted in the (σ, Σ) space (right panel). In the left panel, the level curve of S = 0.001555 is shown by a blue line and the critical curve specified by ﹩{{ \mathcal H }}_{U}\,=﹩−0.614 is shown by a red line. In particular, the region above the critical curve corresponds to libration while the region below it corresponds to circulation. In the right panel, the magnitude of S stands for the area of the shaded region bounded by the isolines of the resonant Hamiltonian. Following the blue line shown in the left panel, particles could switch between libration and circulation regions periodically.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Definition of the adiabatic invariant, S, represented by the area surrounded by isolines of the resonant Hamiltonian in the phase space (σ, Σ) for the case of 1:2 resonance (holding asymmetric libration centers). There are inner and outer separatrices, which are marked by red dashed lines. The Hamiltonian of the inner separatrix is denoted by ﹩{{ \mathcal H }}_{U}^{(1)}﹩ and that of the outer separatrix by ﹩{{ \mathcal H }}_{U}^{(2)}﹩. The upper panels are for the libration cases with tadpole-type trajectories (i.e., ﹩{ \mathcal H }\gt {{ \mathcal H }}_{U}^{(1)}﹩), and the bottom panels are for the libration case with horseshoe-type trajectories (i.e., ﹩{{ \mathcal H }}_{U}^{(1)}\gt { \mathcal H }\gt {{ \mathcal H }}_{U}^{(2)}﹩) and for the circulation case (﹩{ \mathcal H }\lt {{ \mathcal H }}_{U}^{(2)}﹩).
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Level curves of the adiabatic invariant S (i.e., phase portrait) in the secular evolution for TNOs inside 2:5 resonance with Neptune (upper left panel) and time histories of σ and ω of three representative trajectories numerically propagated in the semi-secular model (other three panels). In practical simulations, the maximum inclination is fixed at ﹩{I}_{\max }=30^\circ ﹩ and the resonant Hamiltonian is assumed to be ﹩{ \mathcal H }=\,﹩−0.614. In the phase portrait (see the upper left panel), three numerically integrated trajectories are shown by green lines and numbered 1, 2, and 3, and the critical curve specified by ﹩{{ \mathcal H }}_{U}=\,﹩−0.614 is marked by a red line. It is observed that the numerically propagated trajectories follow closely along the level curves in the phase portrait.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Level curves of the adiabatic invariant S (i.e., phase portrait) in the secular evolution for minor bodies inside 1:2 resonance with Neptune (left panel) and time histories of σ and ω of trajectory D numerically propagated in the semi-secular model (right panel). In the phase portrait (see the left panel), three representative trajectories, denoted by letters A, B, and D, are shown by green lines and the critical curves are marked by red dashed lines. It is noted that the time histories of σ and ω of trajectories A and B have been shown in Figure 6. In the tadpole-type region, the adiabatic invariant S is measured at the trailing island.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Level curves of the adiabatic invariant S (i.e., phase portrait) in the secular evolution for minor bodies inside 1:2 resonance with Neptune (upper left panel) and time histories of σ and ω of three representative trajectories numerically propagated in the semi-secular model (other three panels). In the tadpole-type region, the adiabatic invariant S is measured at the leading island. In the phase portrait (see the upper left panel), three representative trajectories, denoted by letters A, B, and C, are shown by green lines and the critical curves are marked by red dashed lines.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Phase portraits together with the trajectories numerically propagated under the full N-body model for a TNO inside 1:2 resonance with Neptune (1996 TR66) and a TNO inside 1:3 resonance with Neptune (2014 SR373). 1996 TR66 is inside the ZLK resonance, while 2014 SR373 is outside it.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Similar to the upper left panel of Figure 8 but for another two representative TNOs (2005 SD278 and 2015 PD312) inside 2:5 resonance with Neptune. During the considered period of time, these two TNOs are also located inside the ZLK resonance.
Paper: The Von Zeipel–Lidov–Kozai Effect inside Mean Motion Resonances with Applications to Trans-Neptunian Objects
Authors: Hanlun Lei, Jian Li, Xiumin Huang, Muzi Li
Figure caption: Phase portraits together with the trajectories numerically propagated under the full N-body model for two TNOs inside 2:3 resonance with Neptune (Pluto and 2004 HA79). These two TNOs are inside the ZLK resonance: one with ω librating around 90° and the other with ω librating around 270°).
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: A CRIRES+ K-band spectrum of MASCARA-1 and the resulting wavelength calibration error. The top panel shows an extracted blaze-corrected spectrum that has been normalized to match the continuum of a telluric model. Here we used the ExoRES pipeline. The bottom panel shows the wavelength calibration error of the same spectrum as estimated using an MCMC. The data shown here are from the lowest S/N spectrum in the MASCARA-1 b data set (S/N ∼ 100), thus illustrating the worst case for this data set. Regions containing fewer telluric lines produce larger calibration errors. We exclude the two spectra between 2.14 and 2.17 μm from further analysis due to large wavelength calibration errors.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: Resolution estimates for the observations of MASCARA-1 b. We compare the resolution estimate obtained by telluric model fitting using different extractions algorithms. In black we show the predicted resolution using the FWHM of the stellar PSF, where each data point is the median from the different orders. The error bars represent the standard deviation across the different orders. We find the resolution to be above R = 100,000 in all cases.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: S/N as a function of the number of singular values removed. The blue and red curves show the S/N of CO and H2O model injections at the expected orbital parameters, respectively, while the observed signals are shown in black solid lines. The lighter colored lines correspond to 100 random injections in the region K  p  ∈ [100, 300] km s−1 and V sys ∈ [ −100, 100] km s−1. The S/N of the injected models was rescaled to match the S/N of the real signals. The vertical dashed lines show the optimal number of singular values that maximizes the injection S/N at the expected orbital parameters.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: Three regions of a CRIRES+ K-band spectrum of MASCARA-1, showing the general agreement between different extraction methods. The black line is a spectrum extracted using the ExoRES pipeline, while the three other spectra are extracted using the CR2RES pipeline. Here we varied the swath width between 400, 800, and 1600 pixels, shown in blue, orange, and green, respectively. Depending on the swath width, some regions show a varying continuum level and even some spiky artifacts, as can be mainly seen on the right in the top panel. Note that the narrow spectral lines in the middle panel appear slightly deeper in the CR2RES pipeline, while the opposite is true for the saturated lines in the bottom panel.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: Different S/N estimates of the spectra from the MASCARA-1 b observations as discussed in Section 3.4. The left panel shows the median S/N for the different frames as given by both pipelines and the CRIRES+ ETC. The S/N from the ETC is order-wise rescaled such that the flux given by the ETC matches the observed flux. The right panel shows the average S/N for all orders, with a smoothing applied for clarity.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: Spectrum extraction. In the top panel is a section of the raw data of an order with bad pixels marked in white. The middle panel is the model of the observation (S  xy  + P  xy  s  x ), where the white dotted lines indicate the regions where the profile is being interpolated due to low S/N. The bottom panel is the residuals between the observation and the model. The units are ADUs.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: Illustration of the effects of calibration and sky emission subtraction. The top panel shows raw data from the MASCARA-1 b data set of a section of one order. Bad pixels are marked in white. Sky emission lines appear as tilted lines with excess flux. The vertical bands are detector readout artifacts, some of which remain after dark subtraction. The middle panel shows the same data that have been calibrated and where the vertical bands have been estimated and removed by subtraction (before dividing by the flat field). The bottom panel shows the result of sky emission subtraction using the ExoRES pipeline. The units are ADUs.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: Residuals of a small wavelength interval after subtracting the average spectrum. The top panel shows the residuals obtained from the ExoRES pipeline. The middle panel shows the residuals obtained from the CR2RES pipeline using an 800-pixel swath width and with subtract_nolight_rows turned off. The bottom row shows the same as the middle row but with subtract_nolight_rows turned on. The data are from the MASCARA-1 b observation. The units are normalized flux, where the continuum level is set to match the telluric transmission before the average spectrum subtracting.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: A raw FPET frame of detector 1 in the K2166 band, overlaid with horizontal dotted lines representing the order tracing and solid lines representing the tilt of the slit image. For similar figures with other wavelength settings see the CRIRES+ Pipeline Manual (0.9.9).
Paper: India’s First Robotic Eye for Time-domain Astrophysics: The GROWTH-India Telescope
Authors: Harsh Kumar, Varun Bhalerao, G. C. Anupama, Sudhanshu Barway, Judhajeet Basu, Kunal Deshmukh, Kishalay De, Anirban Dutta, Christoffer Fremling, Hrishikesh Iyer, Adeem Jassani, Simran Joharle, Viraj Karambelkar, Maitreya Khandagale, K Adithya Krishna, Sumeet Kulkarni, Sujay Mate, Atharva Patil, DVS Phanindra, Subham Samantaray, Kritti Sharma, Yashvi Sharma, Vedant Shenoy, Avinash Singh, Shubham Srivastava, Vishwajeet Swain, Gaurav Waratkar, Dorje Angchuk, Padma Dorjay, Tsewang Dorjai, Tsewang Gyalson, Sonam Jorphail, Tashi Thsering Mahay, Rigzin Norbu, Tarun Kumar Sharma, Jigmet Stanzin, Tsewang Stanzin, Urgain Stanzin
Figure caption:  r-band light curves of a sample of supernovae observed with the GIT. The left panel shows the core-collapse objects, while the right panel shows the thermonuclear SNe. For SN 2019vxm and SN 2019tua, GIT has missed the peak, and we show the early light curves of SN 1996cb (Qiu et al. 1999) and SN 2005ip (Stritzinger et al. 2012) to understand their possible type. GIT has complemented Zwicky Transient Facility (ZTF) surveys in some phases. For some SNe like SN 2021do and SN 2021gmj, we show the light curves in the ZTF − r band (Bellm et al. 2019).
Paper: India’s First Robotic Eye for Time-domain Astrophysics: The GROWTH-India Telescope
Authors: Harsh Kumar, Varun Bhalerao, G. C. Anupama, Sudhanshu Barway, Judhajeet Basu, Kunal Deshmukh, Kishalay De, Anirban Dutta, Christoffer Fremling, Hrishikesh Iyer, Adeem Jassani, Simran Joharle, Viraj Karambelkar, Maitreya Khandagale, K Adithya Krishna, Sumeet Kulkarni, Sujay Mate, Atharva Patil, DVS Phanindra, Subham Samantaray, Kritti Sharma, Yashvi Sharma, Vedant Shenoy, Avinash Singh, Shubham Srivastava, Vishwajeet Swain, Gaurav Waratkar, Dorje Angchuk, Padma Dorjay, Tsewang Dorjai, Tsewang Gyalson, Sonam Jorphail, Tashi Thsering Mahay, Rigzin Norbu, Tarun Kumar Sharma, Jigmet Stanzin, Tsewang Stanzin, Urgain Stanzin
Figure caption: (a) Limiting magnitude variation of GIT-Andor camera in SDSS u′ g′ r′ i′ z′ bands for 300 s exposures. The g′ and r′ band images are deeper as compared to other bands due to low extinction and have a typical depth of 20.5 mag for 300 s exposure. (b) Photometric uncertainty for sources in various bands, as a function of source magnitude. (c) Photometric accuracy of GIT pipeline, measured as the difference between GIT and catalog magnitudes for all sources discussed in Section 5.3.
Paper: India’s First Robotic Eye for Time-domain Astrophysics: The GROWTH-India Telescope
Authors: Harsh Kumar, Varun Bhalerao, G. C. Anupama, Sudhanshu Barway, Judhajeet Basu, Kunal Deshmukh, Kishalay De, Anirban Dutta, Christoffer Fremling, Hrishikesh Iyer, Adeem Jassani, Simran Joharle, Viraj Karambelkar, Maitreya Khandagale, K Adithya Krishna, Sumeet Kulkarni, Sujay Mate, Atharva Patil, DVS Phanindra, Subham Samantaray, Kritti Sharma, Yashvi Sharma, Vedant Shenoy, Avinash Singh, Shubham Srivastava, Vishwajeet Swain, Gaurav Waratkar, Dorje Angchuk, Padma Dorjay, Tsewang Dorjai, Tsewang Gyalson, Sonam Jorphail, Tashi Thsering Mahay, Rigzin Norbu, Tarun Kumar Sharma, Jigmet Stanzin, Tsewang Stanzin, Urgain Stanzin
Figure caption: GROWTH-India Telescope efficiencies during each phase of operations. Three histograms show the efficiencies for manual mode (blue), semiautomated mode (orange), and automated mode (green). The system is currently running in automated mode with a typical efficiency of ∼80%, which is a noticeable improvement over the manual and semiautomated modes of observation. The low effacing tail in automated mode is due to unsuitable weather conditions and instrument failures.
Paper: India’s First Robotic Eye for Time-domain Astrophysics: The GROWTH-India Telescope
Authors: Harsh Kumar, Varun Bhalerao, G. C. Anupama, Sudhanshu Barway, Judhajeet Basu, Kunal Deshmukh, Kishalay De, Anirban Dutta, Christoffer Fremling, Hrishikesh Iyer, Adeem Jassani, Simran Joharle, Viraj Karambelkar, Maitreya Khandagale, K Adithya Krishna, Sumeet Kulkarni, Sujay Mate, Atharva Patil, DVS Phanindra, Subham Samantaray, Kritti Sharma, Yashvi Sharma, Vedant Shenoy, Avinash Singh, Shubham Srivastava, Vishwajeet Swain, Gaurav Waratkar, Dorje Angchuk, Padma Dorjay, Tsewang Dorjai, Tsewang Gyalson, Sonam Jorphail, Tashi Thsering Mahay, Rigzin Norbu, Tarun Kumar Sharma, Jigmet Stanzin, Tsewang Stanzin, Urgain Stanzin
Figure caption: Light curves of GRB optical afterglow detections by GIT. The light curves of these afterglows in g′ (top left panel), r′ (top right panel), and i′ (bottom left panel) bands have been plotted against the Swift GRB afterglow population taken from Kann et al. (2011). These afterglows span over the full range of Swift GRB afterglow population.
Paper: India’s First Robotic Eye for Time-domain Astrophysics: The GROWTH-India Telescope
Authors: Harsh Kumar, Varun Bhalerao, G. C. Anupama, Sudhanshu Barway, Judhajeet Basu, Kunal Deshmukh, Kishalay De, Anirban Dutta, Christoffer Fremling, Hrishikesh Iyer, Adeem Jassani, Simran Joharle, Viraj Karambelkar, Maitreya Khandagale, K Adithya Krishna, Sumeet Kulkarni, Sujay Mate, Atharva Patil, DVS Phanindra, Subham Samantaray, Kritti Sharma, Yashvi Sharma, Vedant Shenoy, Avinash Singh, Shubham Srivastava, Vishwajeet Swain, Gaurav Waratkar, Dorje Angchuk, Padma Dorjay, Tsewang Dorjai, Tsewang Gyalson, Sonam Jorphail, Tashi Thsering Mahay, Rigzin Norbu, Tarun Kumar Sharma, Jigmet Stanzin, Tsewang Stanzin, Urgain Stanzin
Figure caption: Observation procedure of GIT. The procedure is broadly divided into three blocks: “Planning” of targets (top left block), “Observations” which includes scheduling (right block), and adding additional targets using “Triggers” (lower left block). Observations are automated and are monitored by Slack bots.
Paper: India’s First Robotic Eye for Time-domain Astrophysics: The GROWTH-India Telescope
Authors: Harsh Kumar, Varun Bhalerao, G. C. Anupama, Sudhanshu Barway, Judhajeet Basu, Kunal Deshmukh, Kishalay De, Anirban Dutta, Christoffer Fremling, Hrishikesh Iyer, Adeem Jassani, Simran Joharle, Viraj Karambelkar, Maitreya Khandagale, K Adithya Krishna, Sumeet Kulkarni, Sujay Mate, Atharva Patil, DVS Phanindra, Subham Samantaray, Kritti Sharma, Yashvi Sharma, Vedant Shenoy, Avinash Singh, Shubham Srivastava, Vishwajeet Swain, Gaurav Waratkar, Dorje Angchuk, Padma Dorjay, Tsewang Dorjai, Tsewang Gyalson, Sonam Jorphail, Tashi Thsering Mahay, Rigzin Norbu, Tarun Kumar Sharma, Jigmet Stanzin, Tsewang Stanzin, Urgain Stanzin
Figure caption: An (a, e, i) orbital distribution of all solar system objects observed with GIT. The region between perihelion q = 1.3 au and aphelion Q = 0.983 au demarcates the NEO regime. The orbital parameters of periodic comets with a > 4 au and nonperiodic comets are omitted here.
Paper: India’s First Robotic Eye for Time-domain Astrophysics: The GROWTH-India Telescope
Authors: Harsh Kumar, Varun Bhalerao, G. C. Anupama, Sudhanshu Barway, Judhajeet Basu, Kunal Deshmukh, Kishalay De, Anirban Dutta, Christoffer Fremling, Hrishikesh Iyer, Adeem Jassani, Simran Joharle, Viraj Karambelkar, Maitreya Khandagale, K Adithya Krishna, Sumeet Kulkarni, Sujay Mate, Atharva Patil, DVS Phanindra, Subham Samantaray, Kritti Sharma, Yashvi Sharma, Vedant Shenoy, Avinash Singh, Shubham Srivastava, Vishwajeet Swain, Gaurav Waratkar, Dorje Angchuk, Padma Dorjay, Tsewang Dorjai, Tsewang Gyalson, Sonam Jorphail, Tashi Thsering Mahay, Rigzin Norbu, Tarun Kumar Sharma, Jigmet Stanzin, Tsewang Stanzin, Urgain Stanzin
Figure caption: GROWTH-India Telescope inside the enclosure. The Andor camera is shown mounted on the telescope.
Paper: India’s First Robotic Eye for Time-domain Astrophysics: The GROWTH-India Telescope
Authors: Harsh Kumar, Varun Bhalerao, G. C. Anupama, Sudhanshu Barway, Judhajeet Basu, Kunal Deshmukh, Kishalay De, Anirban Dutta, Christoffer Fremling, Hrishikesh Iyer, Adeem Jassani, Simran Joharle, Viraj Karambelkar, Maitreya Khandagale, K Adithya Krishna, Sumeet Kulkarni, Sujay Mate, Atharva Patil, DVS Phanindra, Subham Samantaray, Kritti Sharma, Yashvi Sharma, Vedant Shenoy, Avinash Singh, Shubham Srivastava, Vishwajeet Swain, Gaurav Waratkar, Dorje Angchuk, Padma Dorjay, Tsewang Dorjai, Tsewang Gyalson, Sonam Jorphail, Tashi Thsering Mahay, Rigzin Norbu, Tarun Kumar Sharma, Jigmet Stanzin, Tsewang Stanzin, Urgain Stanzin
Figure caption: Filter response curves for SDSS prime filter set used at GIT. The effective wavelengths for each filter are shown by vertical dashed lines and their values are quoted at the top of the plot.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Abundances as a function of galactocentric distances. We show with a blue solid line the linear regression for the gas-phase oxygen abundances inferred with the strong-line O3N2 calibration by Pettini & Pagel (2004), using the fluxes by Walsh & Roy (1997). We show with a dashed–dotted orange line our stellar weighted average α-abundance gradient. The blue squares display the depletion-corrected direct oxygen abundances by Hadfield & Crowther (2007).
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: [α/Fe] ratios as a function of [Fe/H] abundances for three different elements shown in the legend. The square symbols show the abundances inferred as part of this work. Blue stars show the MW abundances by Reddy et al. (2003, 2006). Orange stars show the LMC abundances by Van der Swaelmen et al. (2013).
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Color-composite image observed with the FORS1 instrument on the ESO’s Very Large Telescope (VLT). The observations were downloaded from the ESO Science Archive and fully processed by Henri Boffin (ESO). Credit: ESO. The white apertures show the locations of the YMCs studied here, along with NGC 1313–379 from Hernandez et al. (2017).