shooting for (even more!) open cluster chemical …shooting for (even more!) open cluster chemical...

Shooting for (Even More!) Open Cluster Chemical Abundances with The Cannon Amy Ray 1 , Peter M. Frinchaboy III 1 , John Donor 1 , Matthew Melendez 1 1 Department of Physics and Astronomy, Texas Christian University, TCU Box 298840 Fort Worth, Texas 76129 Motivation Many open cluster chemical abundance studies have substantial uncertainties from study to study. A few reasons are due to varying data quality, the type of data, which catalog was used for distances, and different data analysis methods between studies. These differences translate into widely varying results when attempting to determine a chemical abundance gradient across the disk of the Milky Way. In this study, we determined chemical abundances for a set of 63 open clusters based on a uniform system. The Cannon • Stuff The Cannon (named after Annie Jump Cannon who is shown in Figure 2), developed by Ness et al. (2015), offers a unique way to find stellar parameters without having to use any models. Instead, it takes a subset of stars, called a reference set, with known parameters or “labels” and creates a model. This model can be applied to the rest of the set of stars to infer labels for them. The labels used for this study were taken from the Sloan Digital Sky Survey (SDSS) IV/ APOGEE DR16, which observed the same stars as our CTIO/Hydra- based study. Figure 2: Annie Jump Cannon examining a photographic plate. Credit: Harvard- Smithsonian Center for Astrophysics New Open Cluster Values We found [Fe/H] binary results are shown in Table 1. We found average [Fe/H] values for more than 10 open clusters that do not have prior measurements from spectroscopic data. A few of the preliminary results are shown in the table to the right. Comparison to Other Studies Future Work We will combine the clusters from this study with other open clusters from the study by Donor et al. (2019) that are also based on APOGEE data. This will allow us to examine abundance trends in the galactic disk over a larger radius. We also have additional set of open clusters that can be analyzed with The Cannon after completing membership analysis. In order to confirm our results, we compared [Fe/H] cluster values to two high resolution spectroscopic surveys, one by Santos et al. (2009) and another by Reddy et al. (2013;2015). We also compared three clusters with Donor et al. (2019) which is also based on APOGEE data. Three one-to-one plots of comparisons are shown in Figure 4. Figure 4: (a) Comparison to 5 open clusters in common with Santos et al. (2009). (b) Comparison to 5 open clusters in common with Reddy et al. (2013;2015). (c) Comparison to 3 clusters in common with Donor et al. (2019). Acknowledgements Text goes here Funding for this work was provided by the National Science Foundation under grant no. AST-1715662. Open Cluster Sample • References Text goes here •Santos N. C., et al., 2009, A&A, 493, 309 •Ness, M., et al., 2015, ApJ, 808, 16 •Reddy, A. B. S., et al., 2013, MNRAS, 431, 3338 •Reddy, A. B. S., et al., 2015, MNRAS, 450, 4301 •Yong, D., Carney, B. W., & Friel, E. D. 2012, AJ, 144, 95 •Frinchaboy, P. M., & Majewski, S. R. 2008, AJ, 136, 118 Data for clusters used in this research were taken from a study by Frinchaboy & Majewski (2008). Observations were taken using the Blanco 4-m Hydra spectrograph in Chile. Frinchaboy & Majewski (2008) also did membership analysis for each cluster and Figure 1 is an example of the results for M67. Figure 1: Color- magnitude diagram for NGC 2682 (M67). Members used in this study are shown as large black circles. (a) (c) (b)

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Page 1: Shooting for (Even More!) Open Cluster Chemical …Shooting for (Even More!) Open Cluster Chemical Abundances withThe Cannon Amy Ray1, Peter M. Frinchaboy III1, John Donor1, Matthew

Shootingfor(EvenMore!)OpenClusterChemicalAbundanceswith TheCannonAmyRay1,PeterM.FrinchaboyIII1,JohnDonor1,MatthewMelendez1

1DepartmentofPhysicsandAstronomy,TexasChristianUniversity,TCUBox298840FortWorth,Texas76129

Motivation

Stuff

Manyopenclusterchemicalabundancestudieshavesubstantialuncertaintiesfromstudytostudy.Afewreasonsareduetovaryingdataquality,thetypeofdata,whichcatalogwasusedfordistances,anddifferentdataanalysismethodsbetweenstudies.ThesedifferencestranslateintowidelyvaryingresultswhenattemptingtodetermineachemicalabundancegradientacrossthediskoftheMilkyWay.Inthisstudy,wedeterminedchemicalabundancesfora setof63openclustersbasedonauniformsystem.

TheCannon

• Stuff TheCannon(namedafterAnnieJumpCannonwhoisshowninFigure2),developedbyNessetal.(2015),offersauniquewaytofindstellarparameterswithouthavingtouseanymodels.Instead,ittakesasubsetofstars,calledareferenceset,withknownparametersor“labels”andcreatesamodel.Thismodelcanbeappliedtotherestofthesetofstarstoinferlabelsforthem.ThelabelsusedforthisstudyweretakenfromtheSloanDigitalSkySurvey(SDSS)IV/APOGEEDR16,whichobservedthesamestarsasourCTIO/Hydra-basedstudy.

Figure2: AnnieJumpCannonexaminingaphotographicplate.Credit:Harvard-SmithsonianCenterforAstrophysics

NewOpenClusterValues

Wefound[Fe/H]binaryresultsareshowninTable1.Wefoundaverage[Fe/H]valuesformorethan10openclustersthatdonothavepriormeasurementsfromspectroscopicdata.Afewofthepreliminaryresultsareshowninthetabletotheright.

ComparisontoOtherStudies

• Stuff

FutureWork

Wefo

WewillcombinetheclustersfromthisstudywithotheropenclustersfromthestudybyDonoretal.(2019)thatarealsobasedonAPOGEEdata.Thiswillallowustoexamineabundancetrendsinthegalacticdiskoveralargerradius.WealsohaveadditionalsetofopenclustersthatcanbeanalyzedwithTheCannonaftercompletingmembershipanalysis.

Inordertoconfirmourresults,wecompared[Fe/H]clustervaluestotwohighresolutionspectroscopicsurveys,onebySantosetal.(2009)andanotherbyReddyetal.(2013;2015).WealsocomparedthreeclusterswithDonoretal.(2019)whichisalsobasedonAPOGEEdata.Threeone-to-oneplotsofcomparisonsareshowninFigure4.

Figure4:(a)Comparisonto5openclustersincommonwithSantosetal.(2009).(b)Comparisonto5openclustersincommonwithReddyetal.(2013;2015).(c)Comparisonto3clustersincommonwithDonoretal.(2019).

AcknowledgementsTextgoeshereFundingforthisworkwasprovidedbytheNationalScienceFoundationundergrantno.AST-1715662.

OpenClusterSample

• Stuff

ReferencesTextgoeshere•SantosN.C.,etal.,2009,A&A,493,309

•Ness,M.,etal.,2015,ApJ,808,16•Reddy,A.B.S.,etal.,2013,MNRAS,431,3338

•Reddy,A.B.S.,etal.,2015,MNRAS,450,4301•Yong,D.,Carney,B.W.,&Friel,E.D.2012,AJ,144,95•Frinchaboy,P.M.,&Majewski,S.R.2008,AJ,136,118

DataforclustersusedinthisresearchweretakenfromastudybyFrinchaboy&Majewski (2008).ObservationsweretakenusingtheBlanco4-mHydraspectrographinChile.Frinchaboy&Majewski (2008)alsodidmembershipanalysisforeachclusterandFigure1isanexampleoftheresultsforM67.

Figure1:Color-magnitudediagramforNGC2682(M67).Membersusedinthisstudyareshownaslargeblackcircles. (a)

(c)

(b)

BY Kaitlyn Dodge. Group Data Chart ClassFrequency Blue Shooting Stars37 Green Shooting Stars36 Purple Shooting Stars33 Pink Shooting Stars31 Yellow Shooting

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