THE HISTORY OF CHEMICAL ENRICHMENT AND THE SITES OF EARLY NUCLEOSYNTHESIS: CNO ABUNDANCES OF GALACTIC CARBON-ENHANCED METAL-POOR STARS
|
|
- Mark Lambert
- 5 years ago
- Views:
Transcription
1 THE HISTORY OF CHEMICAL ENRICHMENT AND THE SITES OF EARLY NUCLEOSYNTHESIS: CNO ABUNDANCES OF GALACTIC CARBON-ENHANCED METAL-POOR STARS By Catherine R. Kennedy A DISSERTATION Submitted to Michigan State University in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY Physics and Astronomy 2011
2 ABSTRACT THE HISTORY OF CHEMICAL ENRICHMENT AND THE SITES OF EARLY NUCLEOSYNTHESIS: CNO ABUNDANCES OF GALACTIC CARBON-ENHANCED METAL-POOR STARS By Catherine R. Kennedy This dissertation focuses on abundance analyses of carbon-enhanced metal-poor (CEMP) Galactic halo stars. Different methods for determining carbon, nitrogen, oxygen, and also some barium abundances are described. The study of these abundances in such stars serves to investigate the means by which the Universe became enriched in metals. Due to the different kinds of CEMP stars observed in the Milky Way, it can only be assumed that there is certainly more than one method of carbon-enhancement at early times. Complete abundance analyses for as many of these archaeological relics as possible are needed in order to constrain the astrophysical sites of early carbon production. There are three main parts of this dissertation. The first part describes new techniques to determine oxygen abundances from spectra of the near-infrared molecular CO bands. With the near-ir OSIRIS spectrograph on the SOAR 4.1-m telescope, 57 CEMP stars were observed. A wide range of oxygen abundances were estimated, and the results were statistically compared to high-resolution estimates for both carbonenhanced and carbon-normal metal-poor stars. Abundance patterns of the sample stars were compared to yield predictions for very metal-poor asymptotic giant branch (AGB) stars. The majority of the sample exhibit patterns consistent with CEMP stars having s-process-element enhancements, and thus have very likely been polluted by carbon- and oxygen-enhanced material transferred from a metal-poor AGB
3 companion. The second part delineates a new survey effort implemented in order to identify new CEMP stars. For the initial pilot study, a new selection technique was developed based solely on the strength of the CH G band at 4300 Å. This technique eliminated previous temperature and metallicity biases present in other CEMP surveys. Observations of the pilot sample were carried out with the Goodman HTS spectrograph on the SOAR 4.1-m telescope. Of the over 120 candidate stars observed, over 35% were found to be CEMP stars. The selection technique was then improved to include a second index for the strength of the G band, and the survey was continued on both the SOAR and Gemini telescopes. After this extension, the success rate of this program increased to 50%. The final part of this dissertation contains details of a pilot study of known metalpoor stars using the X-Shooter spectrograph on the Very Large Telescope (VLT). With three spectrograph arms (near-ultraviolet, optical, and near-infrared), this instrument was used to calculate carbon, nitrogen, oxygen, and barium abundances for a sample of 27 CEMP stars. The broad spectral range of this instrument is unprecedented, and it is an efficient way to estimate abundances for several pertinent species in just one exposure per star. Of the 27 stars, many proved to be enhanced in carbon. The majority appear to be consistent with s-process-element enhancement, but there was one extremely metal-poor star which falls into the rare family of CEMP stars with no neutron-capture-element enhancement.
4 Copyright by CATHERINE R. KENNEDY 2011
5 To my mother and father for the love and support. To Lauren, Nora, Liz, Amanda, Jennie, Cait, Val, Bill, and Dave for the lasting friendship and the laughter. To the person I have looked up to thoughout my entire life, John. I have always endeavored to be his equal with regard to integrity, work ethic, and academic success. He is as fast now as he was on his Big Wheel; but if I pedal fast, I may catch up to him. v
6 ACKNOWLEDGMENTS Many thanks to Timothy C. Beers for his guidance for the past five years. Special thanks to Silvia Rossi, Vinicius Placco, Thirupathi Sivarani, and Young Sun Lee for endless amounts of collaborative spirit and scientific expertise. C.R.K. acknowledges partial support for this work from grants AST , as well as from PHY and PHY ; Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA), awarded by the US National Science Foundation. Thanks to Christopher Waters for the LATEX class used to format this thesis. vi
7 TABLE OF CONTENTS List of Tables... List of Figures... ix xi List of Symbols... xv 1 Introduction The Milky Way Components and Formation Scenarios The Carbon-Enhanced Metal-Poor Stars of the Galactic Halo. 3 2 Oxygen Abundances for CEMP Stars from Near-Infrared Spectroscopy with SOAR/OSIRIS Introduction Observations and Data Reduction Adopted Atmospheric Parameters and Synthetic Spectra Determination of [O/H] Results Statistical Comparison to High-resolution Oxygen Estimates High-resolution Nitrogen Estimates Discussion [O/Fe] in Carbon-normal and Carbon-enhanced Metal-poor Stars C, N, and O: Comparison with AGB Models Considering the Effects of Dilution Uncertainties of the AGB Models Conclusions A Survey to Identify New CEMP Stars Motivation The Selection Technique: A New Extended Index for the CH G Band Target Selection Observations and Data Reduction Atmospheric Parameters and Carbon Abundances Results Conclusions vii
8 4 Improving the Selection Technique and Extending the Survey with Multiple Observatories Refining the Selection Criteria New Selection Follow-up Observations: GMOS on Gemini Follow-up Observations: Goodman HTS on SOAR Carbon, Nitrogen, Oxygen, and Barium Abundances with XSHOOTER on VLT Introduction Selected Targets and Observations Model Atmospheres, Line Lists, and Synthetic Spectra Model Atmospheres Line Lists Synthetic Spectra Abundance Determinations Results Discussion Neutron-capture-enhanced Stars CEMP-no Stars Conclusions Conclusions A XSHOOTER Spectra: [C/Fe], [N/Fe], [O/Fe], and [Ba/Fe] Determinations A.1 [C/Fe] A.2 [N/Fe] A.3 [O/Fe] A.4 [Ba/Fe] B Acronyms References viii
9 LIST OF TABLES 1.1 Classification of CEMP Stars Atmospheric Parameters and Carbon Abundances I Atmospheric Parameters and Carbon Abundances II Atmospheric Parameters and Carbon Abundances III Abundance Ratios for the Entire Sample I Abundance Ratios for the Entire Sample II Abundance Ratios for the Entire Sample III Classification of CEMP Candidates Color, GPE, and Category of Pilot Stars I Color, GPE, and Category of Pilot Stars II Color, GPE, and Category of Pilot Stars III Color, GPE, and Category of Pilot Stars IV Color, GPE, and Category of Pilot Stars V Color, GPE, and Category of Pilot Stars VI Atmospheric Parameters and Carbon Abundances for Pilot Stars I Atmospheric Parameters and Carbon Abundances for Pilot Stars II Atmospheric Parameters and Carbon Abundances for Pilot Stars III Atmospheric Parameters and Carbon Abundances for Pilot Stars IV Atmospheric Parameters and Carbon Abundances for Pilot Stars V Atmospheric Parameters and Carbon Abundances for Pilot Stars VI Atmospheric Parameters and Carbon Abundances for Gemini Stars I.. 63 ix
10 4.2 Atmospheric Parameters and Carbon Abundances for Gemini Stars II Atmospheric Parameters and Carbon Abundances for Gemini Stars III Atmospheric Parameters and Carbon Abundances for Goodman Stars I Atmospheric Parameters and Carbon Abundances for Goodman Stars II Atmospheric Parameters and Carbon Abundances for Goodman Stars III Atmospheric Parameters and Barium Abundances for X-Shooter Stars I Atmospheric Parameters and Barium Abundances for X-Shooter Stars II Nitrogen, Carbon, and Oxygen Abundances for X-Shooter Stars I Nitrogen, Carbon, and Oxygen Abundances for X-Shooter Stars II x
11 LIST OF FIGURES 1.1 Path of s- and r-process Three synthetic spectra with different [O/Fe] ratios Estimates of [O/Fe] for four stars Distribution of [O/Fe] [O/Fe] vs. [Fe/H] for stars with [C/Fe] [O/Fe] compared to high-resolution analysis C, N, and O abundances vs. metallicity for 10 stars Abundances compared to AGB abundance yields The effects of dilution on abundances The new GPE index GPE vs. (J K) Index-color distribution of CEMP candidates of different types Metallicity cutoff for CEMP candidates Goodman spectra of pilot-program stars I Goodman spectra of pilot-program stars II Goodman spectra of pilot-program stars III [C/Fe] estimate for pilot-program star [C/Fe] versus [Fe/H] for Pilot Sample The new EGP index for 6 HES stars Distribution of GPE and EGP indices for both the stars and the bright subsets xi
12 4.3 Distribution of GPE and EGP indices after the saturation correction Selection criteria for GPE and EGP indices [C/Fe] versus [Fe/H] for Pilot Sample + Gemini Sample [C/Fe] versus [Fe/H] for Pilot + Gemini + Additional Goodman samples C, N, O, and Ba spectral synthesis C, N, O, and Ba abundances Abundance patterns for CEMP X-Shooter stars CNO Abundances of metal-poor AGB Stars A.1 Carbon abundances for X-Shooter stars A.2 Carbon abundances for X-Shooter stars A.3 Carbon abundances for X-Shooter stars A.4 Carbon abundances for X-Shooter stars A.5 Carbon abundances for X-Shooter stars A.6 Carbon abundances for X-Shooter stars A.7 Carbon abundances for X-Shooter stars A.8 Carbon abundances for X-Shooter stars A.9 Carbon abundances for X-Shooter stars A.10 Carbon abundances for X-Shooter stars A.11 Carbon abundances for X-Shooter stars A.12 Carbon abundances for X-Shooter stars A.13 Carbon abundances for X-Shooter stars A.14 Carbon abundances for X-Shooter stars A.15 Nitrogen abundances for X-Shooter stars A.16 Nitrogen abundances for X-Shooter stars xii
13 A.17 Nitrogen abundances for X-Shooter stars A.18 Nitrogen abundances for X-Shooter stars A.19 Nitrogen abundances for X-Shooter stars A.20 Nitrogen abundances for X-Shooter stars A.21 Nitrogen abundances for X-Shooter stars A.22 Nitrogen abundances for X-Shooter stars A.23 Nitrogen abundances for X-Shooter stars A.24 Nitrogen abundances for X-Shooter stars A.25 Nitrogen abundances for X-Shooter stars A.26 Nitrogen abundances for X-Shooter stars A.27 Nitrogen abundances for X-Shooter stars A.28 Nitrogen abundances for X-Shooter stars A.29 Oxygen abundances for X-Shooter stars A.30 Oxygen abundances for X-Shooter stars A.31 Oxygen abundances for X-Shooter stars A.32 Oxygen abundances for X-Shooter stars A.33 Oxygen abundances for X-Shooter stars A.34 Oxygen abundances for X-Shooter stars A.35 Oxygen abundances for X-Shooter stars A.36 Oxygen abundances for X-Shooter stars A.37 Oxygen abundances for X-Shooter stars A.38 Barium abundances for X-Shooter stars A.39 Barium abundances for X-Shooter stars A.40 Barium abundances for X-Shooter stars A.41 Barium abundances for X-Shooter stars xiii
14 A.42 Barium abundances for X-Shooter stars A.43 Barium abundances for X-Shooter stars A.44 Barium abundances for X-Shooter stars A.45 Barium abundances for X-Shooter stars xiv
15 LIST OF SYMBOLS pc unit of distance equal to cm T eff effective temperature g surface gravity M solar mass xv
16 Chapter 1: Introduction There are a variety of methods by which the Universe was polluted with all of the elements that we observe today. Big Bang nucleosynthesis provided the early Universe with only hydrogen, helium, and trace amounts of lithium. All other elements have since been created in stars. As early generations of stars exploded as supernovae, the interstellar medium (ISM) was polluted with the heavy elements that were created within them and during their explosions. Subsequent generations of stars were then born of this more chemically-enriched material. This cycle of the birth and death of generations of stars continues today, and the main result of this process is that the generations of stars become more and more chemically-enriched than their predecessors as time goes on. In order to quantify this process, one can measure the amount of metals in stars via stellar spectroscopy. In astronomical terms, metals are defined as all elements except for hydrogen and helium. In this dissertation, the metallicity of a star is defined as [Fe/H], a logarithmic comparison of the amount of metal in a star compared to that of the Sun. Other abundances will be discussed in terms of the same notation: [A/B] = log(n A /N B ) star log(n A /N B ), (1.1) where N A and N B are the number densities of the elements A and B for the stars. In these terms, a star which has [Fe/H] = 1.0 has a metallicity of 10 times less than solar, a star which has [Fe/H] = 2.0 has a metallicity of 100 times less than solar 1
17 and so on. 1.1 The Milky Way Components and Formation Scenarios The Milky Way consists of several different physical components. The populations of stars that exist in the three main components (the bulge, the disk, and the halo) have different kinematic and chemical properties. The bulge of the galaxy lies directly in the center and rotates with a mean velocity of 75 km/s. The bulge has a mean metallicity of [Fe/H] = +0.25, which is almost twice the solar metallicity. However, the stars in the bulge span a large range in ages and metallicities (from [Fe/H] = 1.50 to +0.50) and therefore have likely originated from different populations of stars (Zoccali et al., 2008). The disk of the Milky Way is composed of several spiral arms and is of course home to the Sun, which is a distance of approximately 8 kpc away from the center of our Galaxy. The disk itself can be subdivided into separate components: the thin disk and the thick disk. The thin disk contains stars which are roughly comparable in composition to the Sun, having metallicities that are typically within ±2 times the solar value. The thick disk is slightly more metal-poor overall, having metallicities that range from 1.6 < [Fe/H] < 0.4. The halo is the site of some of the oldest and most metal-poor stars in the Milky Way. The focus of this dissertation is primarily on these halo stars. Like the disk of the Galaxy, the halo can also be separated into different components which have different characteristics. The inner halo reaches to kpc from the Galactic center. It is slightly oblate, and the stars that populate the inner halo typically have high orbital eccentricities. The mean metallicity of the inner halo is [Fe/H] = 1.6. There is also a counter-rotating outer halo component (at distances of above 15 kpc 2
18 from the Galactic center) which is more spherical and has a mean metallicity of [Fe/H] = 2.2 (Carollo et al., 2007). The different kinematic properties and chemical properties of the two halo components are indicative of different structure formation episodes of the Galactic halo as a whole. According to current theory, the inner halo was most likely formed by the following hierarchical scenario. A merger of several sub-galactic-mass fragments occurred to form the bulk component of the Milky Way. Subsequent merging of other fragments resulted in the formation of the inner halo which then necessarily contained the higheccentricity stars that are observed today. As the disk of the Galaxy grew in size, the surrounding inner halo component was flattened, giving rise to its now-observed oblate shape (Bekki & Chiba, 2001; Chiba & Beers, 2001). As the outer halo is both more metal poor and counter rotating, it is likely to have been formed by another scenario altogether. It is believed that the outer halo was formed from the accretion of much smaller subsystems, such as the ultra-faint dwarf galaxies that are observed today. Upon such accretion, these systems would suffer severe tidal stripping which would result in the field halo stars that are currently present in the outer halo. Indeed, the recently-studied ultra-faint dwarf galaxies exhibit the very low metallicities and abundance patterns similar to outer-halo field stars (Norris et al., 2010a,b). 1.2 The Carbon-Enhanced Metal-Poor Stars of the Galactic Halo Metal-poor stars in the Milky Way are archaeological relics of the Galaxy s formation. By studying the composition of these objects, it is possible to unearth clues to the formation and nucleosynthetic history of the Milky Way. Large-scale survey efforts such as the HK survey (Beers et al., 1985, 1992) and the Hamburg/ESO Survey (HES; 3
19 Christlieb, 2003; Christlieb et al., 2008) have resulted in the identification of very large numbers of metal-poor stars (with [Fe/H] < 1.0). A significant fraction of metalpoor stars are found to be enhanced in carbon (Lucatello et al., 2006; Marsteller et al., 2009), and the fraction of carbon-enhanced metal-poor stars increases with declining metallicity (Beers & Christlieb, 2005; Frebel et al., 2005; Norris et al., 2007). Much can be learned from the stellar spectra of carbon-enhanced metal-poor stars. Carbon-enhanced metal-poor (CEMP) stars preserve chemical signatures of the Galactic past. By studying their abundance patterns, one can begin to uncover details of the origins of the elements. There exist a number of different types of CEMP stars which have unique abundance characteristics. The different classes, as defined by Beers & Christlieb (2005), are listed in Table 1.1. Table 1.1: Classification of CEMP Stars Class Abundance Pattern CEMP [C/Fe] > +1.0 CEMP-r [C/Fe] > +1.0 and [Eu/Fe] > +1.0 CEMP-s [C/Fe] > +1.0, [Ba/Fe] > +1.0, and [Ba/Eu] > +0.5 CEMP-r/s [C/Fe] > +1.0 and 0.0 < [Ba/Fe] < +0.5 CEMP-no [C/Fe] > +1.0 and [Ba/Fe] < 0.0 The different classes of CEMP stars are suggestive of different sites of carbon production at early times. Often, CEMP stars exhibit enhancements of neutron-capture elements. The most common types of carbon-enhanced metal-poor stars observed are the CEMP-s stars, which show evidence of s-process-element enhancements. It is widely believed that these objects are the result of mass transfer from a companion low-metallicity asymptotic giant branch (AGB) star, where the production of carbon 4
20 and s-process-elements occurs. Stars which have r-process enhancements (CEMP-r) might have evolved from the interstellar medium (ISM) that was polluted by early Type II supernovae where the r-process is believed to have occurred. There are even some CEMP stars which have both s- and r-process element enhancements, suggesting that the source of their carbon-enhancements arises from more than one site and/or time period. While there are no true s- or r-process elements, there are certain isotopes of elements which are exclusive to each process. Figure 1.1 shows a portion of the path of the s- and r-processes. Also in Figure 1.1 is the relative fraction of each element that arises from either process. Figure 1.1: Part of the paths of the s- and r-processes. The columns on the right designate the percentage of each element which is populated by the occurrence of each process. This figure is taken from Sneden et al. (2008). For interpretation of the references to color in this and all other figures, the reader is referred to the electronic version of this dissertation. 5
21 For the CEMP-no class, which exhibit NO neutron-capture element enhancements, the source of carbon enhancement is less certain. Current theories include the possibility that very massive, rapidly-rotating, mega metal-poor stars (with [Fe/H] < 6.0) were very efficient producers of carbon, nitrogen, and oxygen (Hirschi et al., 2006; Meynet et al., 2006). Yet another possible source of CNO enhancement for the observed CEMP-no stars are faint supernovae which undergo heavy mixing and fallback during their explosions (Umeda & Nomoto, 2003, 2005; Tominaga et al., 2007). The majority of CEMP-no stars tend to be some of the most metal-poor objects observed. In fact, they are likely the preservers of the earliest form of carbon production that occurred in the first generations of stars. This idea is confirmed by the recent discovery of a carbon-enhanced, extremely metal-poor damped Ly-α system at a redshift of z = 2.34 (Cooke et al., 2011). The abundances determined by this study are consistent with observed CEMP-no stars in the Galactic halo. By estimating carbon, nitrogen, oxygen, and neutron-capture-element abundances, one can classify CEMP stars and begin to constrain the properties of Galactic Chemical Evolution (GCE). Constraints can also be applied to the Initial Mass Function (IMF) of the Galaxy, as information is revealed about the distribution of different progenitors of CEMP stars and their masses. The organization of this dissertation is as follows. Chapter 2 is a version of the published paper of Kennedy et al. (2011, reproduced by permission of the AAS), and reports new oxygen abundances for known CEMP stars. Chapters 3 and 4 describe a new, highly-successful technique to discover previously-unidentified Galactic CEMP stars. The determinations of C, N, O, and Ba abundances for CEMP stars with the new X-Shooter spectrograph are presented in chapter 5, and the conclusions related to all of these studies are discussed in chapter 6. 6
22 Chapter 2: Oxygen Abundances for CEMP Stars from Near-Infrared Spectroscopy with SOAR/OSIRIS 2.1 Introduction Carbon-enhanced metal-poor (CEMP) stars are quite common in the halo populations of the Milky Way, and are of particular interest, as they preserve important astrophysical information concerning the early chemical evolution of the Galaxy (Beers & Christlieb, 2005). Previous work has indicated that at least 20% of stars with metallicities [Fe/H] < 2.0 exhibit large overabundances of carbon ([C/Fe] > +1.0; Lucatello et al., 2006; Marsteller et al., 2009), although recent studies (e.g. Cohen et al., 2005; Frebel et al., 2006), have claimed that this fraction is somewhat lower (9% and 14%, respectively, for [Fe/H] < 2.0). In any case, the fraction of CEMP stars rises to 30% for [Fe/H] < 3.0, 40% for [Fe/H] < 3.5, and 100% for [Fe/H] < 4.0 (Beers & Christlieb, 2005; Frebel et al., 2005; Norris et al., 2007). There exist a number of classes of CEMP stars, some of which have been associated with proposed progenitor objects. CEMP-s stars (those with s-process-element enhancement), for example, are the most commonly observed type to date. Highresolution spectroscopic studies have revealed that around 80% of CEMP stars exhibit s-process-element enhancement (Aoki et al., 2007). The favored mechanism 7
23 invoked to account for these stars is mass transfer of carbon-enhanced material from the envelope of an asymptotic giant branch (AGB) star to its binary companion; it is this surviving binary companion that is now observed as a CEMP-s star. The class of CEMP-no stars (which exhibit no strong neutron-capture-element enhancements) is particularly prevalent among the most metal-poor stars. Possible progenitors for this class include massive, rapidly rotating, mega metal-poor ([Fe/H] < 6.0) stars, which models suggest have greatly enhanced abundances of CNO due to distinctive internal burning and mixing episodes, followed by strong mass loss (Meynet et al., 2006; Hirschi et al., 2006; Meynet et al., 2010). Another suggested mechanism is pollution of the interstellar medium by the so-called faint supernovae associated with the first generations of stars, which experience extensive mixing and fallback during their explosions (Umeda & Nomoto, 2003, 2005; Tominaga et al., 2007); high [C/Fe] and [O/Fe] ratios are predicted in the ejected material. This model well reproduces the observed abundance pattern of the CEMP-no star BD+44:493, the ninth-magnitude [Fe/H] = 3.7 star (with [C/Fe]= +1.3, [N/Fe] = +0.3, and [O/Fe] = +1.6) discussed by Ito et al. (2009). The great majority of known CEMP stars were originally identified as metal-poor candidates from objective-prism surveys, such as the HK Survey (Beers et al., 1985, 1992), and the Hamburg/ESO Survey (HES; Christlieb, 2003; Christlieb et al., 2008), based on a weak (or absent) Ca II K line. Some candidate CEMP stars also come from a list of HES stars selected from the prism plates based on their strong molecular lines of carbon (Christlieb et al., 2001). Medium-resolution spectra for most of these objects have been obtained over the past few years (Goswami et al., 2006, 2010; Marsteller, 2007, T. Sivarani et al. 2011, in preparation). Inspection of these data indicates that at least 50% of these targets are consistent with identification as CEMP stars, while the others are roughly solar-metallicity carbon-rich stars. Dedicated surveys for CEMP stars covering a wide range of carbon abundance and metallicities 8
24 are just now getting underway, based on the observed strength of the CH G band measured from the HES prism plates (e.g., Placco et al., 2010). In order to more fully test the association of CEMP-no stars with massive primordial stars and/or faint supernovae, and to better explore the nature of the s-process in low-metallicity AGB stars (which is still rather poorly understood; Herwig, 2005), we require measurements of the important elements C, N, and O for as large a sample of CEMP stars as possible. While estimates of carbon and nitrogen abundances can be determined from medium-resolution optical or near-ultraviolet spectra of CEMP stars (e.g., Rossi et al., 2005; Beers et al., 2007b; Johnson et al., 2007; Marsteller et al., 2009), high-resolution spectroscopy is usually required in order to obtain estimates of oxygen abundances from the forbidden [O1] λ6300 line, the λ7700 triplet (e.g., Schuler et al., 2006; Sivarani et al., 2006; Fabbian et al., 2009, and references therein), or the OH lines at µm (Meléndez & Barbuy, 2002). Masseron et al. (2010) provide a useful compilation of known elemental abundances for CEMP stars. In addition to abundance measurements for metal-poor halo stars, oxygen abundances have also been measured directly in the gas phase in damped Lyα systems (Pettini et al., 2002, 2008). If a star has a measured carbon abundance (and, assuming C/O > 1, which applies for most CEMP stars), essentially all of the O is locked up in CO molecules, and medium-resolution spectroscopy of the CO ro-vibrational bands in the near-infrared (near-ir) can be used for the estimation of [O/Fe] (e.g., Beers et al., 2007b, and references therein). Although one sacrifices measurement accuracy, relative to highresolution studies, this approach has the great advantage that medium-resolution spectroscopy can be gathered far faster than high-resolution spectroscopy, ensuring that much larger samples of stars can be investigated. In addition, the large separation of the 13 CO lines from the 12 CO lines at 2.3µm provides a straightforward means to measure the important mixing diagnostic 12 C/ 13 C, as long as the signal-to-noise ratio 9
25 (S/N) of the spectra is sufficient. This paper is outlined as follows. In Section 2.2, we discuss details of the observations and data reduction procedures used in the present study. Section 2.3 describes the previously determined atmospheric parameter estimates and their origins, as well as details about the synthetic spectra. Methods used for the determination of [O/Fe] for our sample of stars are described in Section 2.4. Our results and a statistical comparison to high-resolution estimates of [C/Fe] and [O/Fe] for a subset of our program stars can be found in Section 2.5. Section 2.6 is a short discussion of our results; conclusions follow in Section Observations and Data Reduction Our sample of 57 stars was selected from the HES, based on follow-up mediumresolution optical spectra obtained during the course of searches for low-metallicity stars. These optical spectra were obtained with the GOLDCAM spectrograph on the KPNO 2.1m telescope and with the RC Spectrographs on the 4m KPNO and CTIO telescopes (see Beers et al., 2007b, hereafter Paper I). Additional targets were selected from the list of carbon-rich candidates published by Christlieb et al. (2001) with available optical spectra. Based on the optical spectra, all of the candidates are metal-poor stars, spanning the metallicity range 2.8 [Fe/H] 1.0. All of the stars were selected to be carbon-rich, with the majority exhibiting [C/Fe] +1.0, and thus are carbon enhanced as defined by Beers & Christlieb (2005). Since our intention was to obtain near-ir spectroscopy of the CO features, the stars were also selected to have effective temperatures less than 5000 K, since warmer stars do not exhibit strong CO. Estimates of [O/Fe] for our program stars are derived from the analysis of mediumresolution near-ir spectra taken with the SOAR 4.1m telescope, using the OSIRIS (Ohio State Infrared Imager/Spectrometer; Depoy et al., 1993) spectrograph during 10
26 2005 October to 2008 June. We used the long slit (width set to 1 ) and long camera (with focal ratio f/7), which provided a resolving power R = The long-pass K-band filter was used to isolate the spectral region from 2.25µm to 2.45µm. Visible in this band are the four ro-vibrational CO features used for the determination of [O/Fe]. We also observed A0-type stars at the same air mass as the observations of the program objects in order to correct for the presence of telluric lines in the spectra. The K-band magnitude range for our sample stars is 7 12, resulting in exposure times in the range seconds in order to reach our targeted S/N of 50/1. Spectra of Ar Ne arc lamps, taken before or after each program star, were used for the wavelength calibration of our sample. Bias correction, flat-fielding, spectral extraction, wavelength calibration, telluric feature correction, and continuum normalization were all performed using standard IRAF packages. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. 2.3 Adopted Atmospheric Parameters and Synthetic Spectra Atmospheric parameters (T eff, log g, and [Fe/H]) were estimated from available optical and near-ir photometry as well as from previously obtained medium-resolution optical spectroscopy. Estimates of T eff are obtained from measured V K colors (taken from Beers et al., 2007a, and references therein, as well as from the 2MASS Point Source Catalog; Skrutskie et al. 2006). The use of near-ir photometry provides for a more accurate determination of T eff, as the K band is less influenced by the presence of carbon features than bluer bands. We used the Alonso et al. (1996) calibrations of T eff with V K colors, as described in Paper I. Surface gravities, 11
27 log g, have been estimated based on the Padova evolutionary tracks for metallicities [Fe/H]= 2.5 and [Fe/H]= 1.7 (Girardi et al., 2000; Marigo et al., 2001). Uncertainties in T eff and log g are 100 K and 0.5 dex, respectively. The microturbulence is taken to be 2 km s 1 for all stars. This is consistent with previously determined microturbulence values for giant CEMP stars (Johnson et al., 2007; Aoki et al., 2007). We have constructed two sets of synthetic spectral templates, covering the optical and near-ir bands. Each set consists of 2000 synthetic spectra with carbon-enhanced atmospheres generated with the MARCS code (Gustafsson et al., 2008). We used a previous generation of models here, as updated CEMP models were not available. We do not, however, anticipate large differences in the models of spectra. The use of carbon-enhanced models is of particular importance for cool CEMP stars, for which the atmospheric structure is significantly altered by carbon (Masseron et al., 2006). No 3D 1D corrections have been applied to our estimates. Recent studies of these effects on two hyper metal-poor stars (Collet et al., 2006) have revealed [O/Fe] corrections of 0.8 based on OH molecules, thereby lowering the measured abundance of oxygen. However, the magnitude of such corrections is expected to decrease with increasing metallicity (Collet et al., 2007). As the metallicities of our targets range from 1.0 to 2.8, it is likely that the three-dimensional effects are less severe. In addition, more recent studies have been carried out (A. Ivanauskas, private communication) concerning the effects of convection on C 2, CH, CN, CO, NH, and OH molecules. When compared to the results from Collet et al. (2006), the magnitude of the corrections appears smaller. The synthetic grid covers a range T eff = 4000 to 6000 K, log g = 0.0 to 5.0, [Fe/H] = 5.0 to 0.0, and [C/Fe] = 0.0 to We adopt fixed nitrogen abundances set to 0.5 dex less than the carbon abundances, which is roughly appropriate for CEMP stars. The CH and CN line lists used for the synthesis of the optical spectra are those compiled by Plez (see Plez & Cohen, 2005). The CO line lists used for the near-ir 12
28 synthesis are taken from Kurucz (1993). The synthetic grids are then degraded to match the resolving power of the observed spectra (R = 2000 for the optical spectra and R = 3000 for the near-ir spectra). The optical spectra are used for the determination of [Fe/H] and [C/H]. The Ca II K line is matched with the model spectra to estimate [Fe/H], and the C 2 and CN features are fit for the estimation of [C/H] (see Paper I). Our adopted atmospheric parameters, as well as the derived [C/H] and [C/Fe], are listed in Tables 2.1, 2.2, and 2.3. Table 2.1: Atmospheric Parameters and Carbon Abundances I Name Teff (K) log g (cgs) [Fe/H] [C/H] [C/Fe] HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE
29 Table 2.2: Atmospheric Parameters and Carbon Abundances II Name Teff (K) log g (cgs) [Fe/H] [C/H] [C/Fe] HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE
30 Table 2.3: Atmospheric Parameters and Carbon Abundances III Name Teff (K) log g (cgs) [Fe/H] [C/H] [C/Fe] HE HE HE HE HE HE HE HE HE HE HE HE HE HE Determination of [O/H] In order to determine [O/H], we employed the near-ir synthetic spectra constructed from model atmospheres with carbon enhancements (see above). Each synthetic spectrum covers the wavelength range 2.25µm 2.40µm. For all combinations of these parameters, models were available with [O/Fe] values of 0.0, +0.4, and The first step in the determination of [O/Fe] is to use the grid of synthetic spectra in combination with the atmospheric parameters to create three models with [O/Fe] 15
31 values of 0.0, +0.4, and These models are then used in order to estimate the [O/Fe] of the program stars. Each star in the sample has a previously estimated T eff, log g, [Fe/H], and [C/Fe]. Given the fact that four parameters are known, the routine begins with 48 models: 16 models for each value of [O/Fe]. The 48 models are selected as having the two closest values of T eff, log g, [Fe/H], and [C/Fe] for each of the three values of [O/Fe]. Once selected, a linear interpolation over each parameter is performed in order to create three final models, one for each value of [O/Fe], with the known values of the four parameters. The three final models for a set of typical atmospheric parameters are shown in Figure 2.1. With the other parameters fixed, it is easy to see how a typical spectrum changes with increasing oxygen abundance. Next, a linear interpolation over [O/Fe] is performed on the three final models, creating new model spectra with varying oxygen. It should be noted that while the interpolation was performed over [O/Fe], the metallicity is fixed, and therefore the oxygen varies as [O/H]. In some cases, it was necessary to extrapolate beyond the boundaries of the model grid in order to find a good fit to the data. Due to the presence of four large CO bands in the near-ir spectra, there were difficulties in fitting the continuum across the entire region. It was important to fit the continua with a low-order function so that the depth of the absorption features was not artificially enhanced or lessened due to the continuum fit. For this reason, the spectra of all stars in the sample were trimmed around each of four CO bands, and a local continuum was fit for each band prior to spectral synthesis. With the use of the synthetic spectra, oxygen abundances were then estimated individually for each of the four bands by minimizing χ 2. A robust average using bisquare weighting of the four separate values was taken as the final estimate of oxygen abundance, with an associated robust estimate of the scatter in these values taken as the error of determination. Figure 2.2 shows the fitting technique applied to four stars from the sample. Each 16
32 Figure 2.1: Three synthetic spectra with different [O/Fe] ratios. Each spectrum has T eff of 4500 K, log g of 1.0, [Fe/H] of 2.0, and [C/Fe] of row shows the four separate estimates of [O/H] for each star. Also plotted on each panel are synthetic spectra with [O/H] values that vary from the best-fitting spectra by ±0.5 dex. Once the robust average is applied the resulting estimates of [O/H] are 1.2 for HE , 0.5 for HE , 0.6 for HE , and 1.2 for HE Results The distributions of [O/Fe] versus three of the parameters used for their determinations are shown in Figure 2.3. The solid lines are linear fits to the data. For the entire sample, there are no significant correlations of [O/Fe] with T eff, [Fe/H], or [C/Fe]. In the middle panel of Figure 2.3, it can be seen that only one of the stars in our sample with [Fe/H] < 2.5 has a value of [O/Fe] less than The bottom panel of Figure 17
33 Figure 2.2: Each row shows four estimates of [O/H] for a star from our sample: HE , HE , HE , and HE , respectively. In each panel, the black lines are the data, the red lines are the best-fitting synthetic spectra, the green lines have [O/H] values of 0.5 dex lower than the best-fitting spectra, and the blue lines have [O/H] values of 0.5 dex higher than the best-fitting spectra. A robust average of the four separate estimates is taken as the final estimate of oxygen abundance for each star. See the text for details. 2.3 shows the distribution of [O/Fe] versus [C/Fe], revealing that the majority of our sample (45 stars) have [C/Fe] > +1.0, and so meet the definition for CEMP stars given by Beers & Christlieb (2005). The other stars exhibit carbon enhancements of [C/Fe] +0.5 and thus are at least moderately enhanced in carbon. The average error in the determination of [O/Fe] for our entire sample is 0.4 dex. We adopted a minimum error for our [O/Fe] estimates of 0.25 dex due to the influence of errors that arise from the estimation of T eff, log g, [Fe/H], and [C/Fe] (see Paper I for details). In Figure 2.4, a carbon cut has been made, such that only the oxygen abundances 18
34 Figure 2.3: Top panel: [O/Fe] vs. T eff for the entire sample. Middle panel: [O/Fe] vs. [Fe/H] for the entire sample. Bottom panel: [O/Fe] vs. [C/Fe] for the entire sample. for those stars with [C/Fe] > are plotted against [Fe/H]. The stars with the highest abundances of carbon exhibit some of the lowest metallicities in our sample. This is not surprising, given that high values of [C/Fe] are often associated with lower metallicities. The fit to the data shows a slight trend of increasing oxygen with decreasing metallicity. The solid line is a least squares fit of [O/Fe] as a function of [Fe/H]. Only a marginally significant slope ( ± 0.314) is found, hence the correlation is quite weak. For comparison, the dashed line in this figure represents the fit of [O/Fe] versus [Fe/H] for the carbon-normal stars from the Spite et al. (2005) sample. The [O/Fe] estimates of the Spite et al. (2005) sample come from the forbidden O I λ6300 line. 19
35 Figure 2.4: [O/Fe] vs. [Fe/H] for the stars with [C/Fe] The dashed line represents the fit for the carbon-normal stars from the Spite et al. (2005) sample of very metal-poor stars, while the solid line is the best fit for our data Statistical Comparison to High-resolution Oxygen Estimates The present catalog of measured oxygen abundances available in the literature for CEMP stars is still relatively small, due to the difficulty of obtaining estimates from optical spectra, even at high spectral resolution. However, we can at least compare the regions of the [O/Fe] versus [Fe/H] parameter space that are occupied by CEMP stars of various sub-classes, based on previous high-resolution oxygen estimates, with those from our present medium-resolution effort. Figure 2.5 shows [O/Fe] for our entire sample, with different boxes indicating the regions of parameter space occupied by several classes of CEMP stars. Sources for 20
36 the high-resolution data for different classes of CEMP stars can be found in Masseron et al. (2010), and references therein. The majority of the stars in our sample occupy regions of the diagram as CEMP stars that have confirmed, high-resolution measurements of s-process-element enhancements. There is clearly overlap with the region occupied by CEMP-r/s stars as well. Few of our stars overlap with the region occupied by CEMP-no stars in the literature; CEMP-no stars tend to be more metal-deficient than most of the stars in our sample. Figure 2.5: [O/Fe] vs. [Fe/H] for the entire sample. The colored boxes show the regions occupied by different types of CEMP stars found in Masseron et al. (2010) High-resolution Nitrogen Estimates For 13 of our program stars, high-resolution estimates of [N/Fe] are available from S. Lucatello (private communication) and/or Aoki et al. (2007). We selected 10 of these 21
37 stars for which the available high-resolution estimates of [C/Fe] were within 0.5 dex of our medium-resolution estimates. The three that are omitted from our analysis and discussion have associated high-resolution [Fe/H] and/or [C/H] estimates that differ significantly from the medium-resolution estimates of these species. We report values of high-resolution [C/Fe], [C/Fe] h, using our estimates of [Fe/H] combined with the high-resolution [C/H]. We report high-resolution estimates of [N/Fe], [N/Fe] h, by combining our estimates of [Fe/H] with the high-resolution values of [N/H]. Two of the 10 stars had high-resolution estimates both from Lucatello and Aoki et al. (2007), and an average of the two available estimates was taken. The values of [C/Fe], [C/Fe] h, [N/Fe] h, [O/Fe], and σ [O/Fe] for our entire sample are listed in Tables 2.4, 2.5, and 2.6. Table 2.4: Abundance Ratios for the Entire Sample I Name [C/Fe] [C/Fe]h [N/Fe]h [O/H] [O/Fe] σ([o/f e]) HE HE HE HE HE HE HE HE HE HE HE HE HE HE
38 Table 2.5: Abundance Ratios for the Entire Sample II Name [C/Fe] [C/Fe]h [N/Fe]h [O/H] [O/Fe] σ([o/f e]) HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE
39 Table 2.6: Abundance Ratios for the Entire Sample III Name [C/Fe] [C/Fe]h [N/Fe]h [O/H] [O/Fe] σ([o/f e]) HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE HE Discussion We expect that the majority of CEMP stars in our sample have been polluted by a companion low-metallicity AGB star. In an AGB star, intershell oxygen is predicted 24
Sara Lucatello Osservatorio Astronomico di Padova, Vicolo dell Osservatorio 5, 35122, Padova, Italy
The Frequency of Carbon-Enhanced Stars in HERES and SDSS Dept. of Physics & Astronomy and JINA: Joint Institute for Nuclear Astrophysics, Michigan State University, E. Lansing, MI 48824 USA E-mail: beers@pa.msu.edu
More informationObservational Constraints on the r-process from Halo r-ii Stars
The Joint Institute for Nuclear Astrophysics Center for the Evolution of the Elements Observational Constraints on the r-process from Halo r-ii Stars Timothy C. Beers University of Notre Dame ND Group:
More informationCarbon Enhanced Metal Poor (CEMP) Stars and the Halo System of the Milky Way
Carbon Enhanced Metal Poor (CEMP) Stars and the Halo System of the Milky Way Daniela Carollo Sydney Castiglione della Pescaia September 2013 Carbon Enhanced Metal Poor Stars (CEMP) CEMP = Carbon Enhanced
More informationBack to the Future: The HK Survey of Beers, Preston, & Shectman
Back to the Future: The HK Survey of Beers, Preston, & Shectman Timothy C. Beers National Optical Astronomy Observatory { SDSS t Galactic Chemical Evolution [Fe/H]= 0 [Fe/H]= 4 [Fe/H]= 5.3 [Fe/H] = - The
More information(Present and) Future Surveys for Metal-Poor Stars
(Present and) Future Surveys for Metal-Poor Stars Timothy C. Beers Department of Physics & Astronomy Michigan State University & JINA: Joint Institute for Nuclear Astrophysics SDSS 1 Why the Fascination
More informationNumber of Stars: 100 billion (10 11 ) Mass : 5 x Solar masses. Size of Disk: 100,000 Light Years (30 kpc)
THE MILKY WAY GALAXY Type: Spiral galaxy composed of a highly flattened disk and a central elliptical bulge. The disk is about 100,000 light years (30kpc) in diameter. The term spiral arises from the external
More informationThorium (Th) Enrichment in the Milky Way Galaxy
Thorium (Th) Enrichment in the Milky Way Galaxy National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan E-mail: aoki.wako@nao.ac.jp Satoshi Honda Kwasan Observatory, Kyoto
More informationCharacterization of the exoplanet host stars. Exoplanets Properties of the host stars. Characterization of the exoplanet host stars
Characterization of the exoplanet host stars Exoplanets Properties of the host stars Properties of the host stars of exoplanets are derived from a combination of astrometric, photometric, and spectroscopic
More informationGALAXIES 626. The Milky Way II. Chemical evolution:
GALAXIES 626 The Milky Way II. Chemical evolution: Chemical evolution Observation of spiral and irregular galaxies show that the fraction of heavy elements varies with the fraction of the total mass which
More informationAbundance Constraints on Early Chemical Evolution. Jim Truran
Abundance Constraints on Early Chemical Evolution Jim Truran Astronomy and Astrophysics Enrico Fermi Institute University of Chicago Argonne National Laboratory MLC Workshop Probing Early Structure with
More informationJINA Observations, Now and in the Near Future
JINA Observations, Now and in the Near Future Timothy C. Beers Department of Physics & Astronomy Michigan State University & JINA: Joint Institute for Nuclear Astrophysics Examples SDSS-I, II, and III
More informationPoS(NIC XII)193. Heavy elements in the early Galaxy. Terese Hansen University of Heidelberg, ZAH, LSW
University of Heidelberg, ZAH, LSW E-mail: thansen@lsw.uni-heidelberg.de Johannes Andersen Niels Bohr Institute, University of Copenhagen E-mail: ja@astro.ku.dk Birgitta Nordtrom Niels Bohr Institute,
More informationBasics of Galactic chemical evolution
Basics of Galactic chemical evolution The chemical abundances of stars provide important clues as to the evolutionary history of a galaxy. Astronomers usually refer to chemical elements other than hydrogen
More informationThe impact of stellar rotation on the CNO abundance patterns in the Milky Way at low metallicities
The impact of stellar rotation on the CNO abundance patterns in the Milky Way at low metallicities Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I - 34131 Trieste, Italia E-mail: Christina.Chiappini@obs.unige.ch
More informationCHEMICAL ABUNDANCE ANALYSIS OF RC CANDIDATE STAR HD (46 LMi) : PRELIMINARY RESULTS
Dig Sites of Stellar Archeology: Giant Stars in the Milky Way Ege Uni. J. of Faculty of Sci., Special Issue, 2014, 145-150 CHEMICAL ABUNDANCE ANALYSIS OF RC CANDIDATE STAR HD 94264 (46 LMi) : PRELIMINARY
More informationUniverse Now. 9. Interstellar matter and star clusters
Universe Now 9. Interstellar matter and star clusters About interstellar matter Interstellar space is not completely empty: gas (atoms + molecules) and small dust particles. Over 10% of the mass of the
More informationin the Milky NOW Way AND and THEN dwarf galaxies Stefania Salvadori
CARBON-ENHANCED DWARF GALAXIES: METAL-POOR STARS in the Milky NOW Way AND and THEN dwarf galaxies Stefania Salvadori University of Groningen Kapteyn Astronomical Institute Netherlands Organization for
More informationBridging the near and the far: constraints on first star formation from stellar archaeology. Raffaella Schneider Sapienza University of Rome
Bridging the near and the far: constraints on first star formation from stellar archaeology Raffaella Schneider Sapienza University of Rome Kyoto,First Stars IV 2012 Kyoto,First Stars IV 2012 "As we extend
More informationBUILDING GALAXIES. Question 1: When and where did the stars form?
BUILDING GALAXIES The unprecedented accuracy of recent observations of the power spectrum of the cosmic microwave background leaves little doubt that the universe formed in a hot big bang, later cooling
More informationLecture 11: Ages and Metalicities from Observations A Quick Review
Lecture 11: Ages and Metalicities from Observations A Quick Review Ages from main-sequence turn-off stars Main sequence lifetime: lifetime = fuel / burning rate $ M " MS = 7 #10 9 % & M $ L " MS = 7 #10
More information金属欠乏星の r プロセス元素組成. r-process abundance of metal-poor stars
金属欠乏星の r プロセス元素組成 r-process abundance of metal-poor stars 本田敏志 Satoshi Honda Center for Astronomy, Univ. of Hyogo Nishi-Harima Astronomical Observatory 初代星 初代銀河研究会 2017@ 呉 2018.2.10-12 Stellar abundances
More informationThe Detailed Abundance Patterns of Light Neutron-Capture Elements in Very Metal-Poor Stars
The Detailed Abundance Patterns of Light Neutron-Capture Elements in Very Metal-Poor Stars 1, Wako Aoki 1, Yuhri Ishimaru 2, Shinya Wanajo 3, Sean G. Ryan 4, Toshitaka Kajino 1, Hiroyasu Ando 1, and Timothy
More informationThe Galactic Halo As Seen By The Hamburg/ESO Survey. Judy Cohen (Caltech)
The Galactic Halo As Seen By The Hamburg/ESO Survey Judy Cohen (Caltech). on behalf of Norbert Christlieb, Tim Beers, Andy McWilliam, Ian Thompson, Steve Shectman, John Norris, and many others Back to
More informationThe first stars: a classification of CEMP-no stars. André Maeder and Georges Meynet ABSTRACT
A&A 580, A32 (2015) DOI: 10.1051/0004-6361/201526234 c ESO 2015 Astronomy & Astrophysics The first stars: a classification of CEMP-no stars André Maeder and Georges Meynet Geneva Observatory, Geneva University,
More informationarxiv:astro-ph/ v1 26 Sep 2006
Carbon Enhanced Metal-Poor Stars. I. Chemical Compositions of 26 Stars 1 Wako Aoki 2, Timothy C. Beers 3, Norbert Christlieb 4, John E. Norris 5, Sean G. Ryan 6,7, Stelios Tsangarides 6 arxiv:astro-ph/0609702v1
More informationEvolution, Death and Nucleosynthesis of the First Stars
First Stars IV, Kyoto, Japan, May 24, 2012 Alexander Heger Stan Woosley Ken Chen Pamela Vo Bernhad Müller Thomas Janka Candace Joggerst http://cosmicexplosions.org Evolution, Death and Nucleosynthesis
More informationChemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia
Chemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia J. Andersen 1,2, B. Nordström 1,2 1 Dark Cosmology Centre, The Niels Bohr Institute, University of Copenhagen, Denmark 2 Stellar Astrophysics
More informationExtremely Metal-Poor Stars
ngcfht workshop 2013.3.27-29. Extremely Metal-Poor Stars Wako Aoki National Astronomical Observatory of Japan Extremely Metal-Poor (EMP) Stars Chemical composition of EMP stars Nucleosynthesis of first
More informationDust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.
More abs. Dust [1.1] kev V Wavelength Optical Infra-red More abs. Wilms et al. 000, ApJ, 54, 914 No grains Grains from http://www.astro.princeton.edu/~draine/dust/dustmix.html See DraineH 003a, column
More information1 Stellar Abundances: The r-process and Supernovae
1 Stellar Abundances: The r-process and Supernovae JOHN J. COWAN Department of Physics and Astronomy, University of Oklahoma Norman, OK 73019, USA CHRISTOPHER SNEDEN Department of Astronomy and McDonald
More informationTHE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS. B. Barbuy
THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS B. Barbuy IAG - Universidade de São Paulo Outline: Interest of studies on Galactic bulge and globulars Data available on metallicity,, kinematics in field
More informationSkyMapper and EMP stars
SkyMapper and EMP stars Mike Bessell on behalf of the EMP team Research School of Astronomy & Astrophysics Slide 2 The discovery of the ancient star with no Fe lines. SkyMapper 2.3m WiFeS Magellan MIKE
More informationSTELLAR HEAVY ELEMENT ABUNDANCES AND THE NATURE OF THE R-PROCESSR. JOHN COWAN University of Oklahoma
STELLAR HEAVY ELEMENT ABUNDANCES AND THE NATURE OF THE R-PROCESSR JOHN COWAN University of Oklahoma First Stars & Evolution of the Early Universe (INT) - June 19, 2006 Top 11 Greatest Unanswered Questions
More informationDetermination of [α/fe] and its Application to SEGUE F/G Stars. Young Sun Lee
Determination of [α/fe] and its Application to SEGUE F/G Stars Young Sun Lee Research Group Meeting on June 16, 2010 Outline Introduction Why [α/fe]? Determination of [α/fe] Validation of estimate of [α/fe]
More information10/26/ Star Birth. Chapter 13: Star Stuff. How do stars form? Star-Forming Clouds. Mass of a Star-Forming Cloud. Gravity Versus Pressure
10/26/16 Lecture Outline 13.1 Star Birth Chapter 13: Star Stuff How do stars form? Our goals for learning: How do stars form? How massive are newborn stars? Star-Forming Clouds Stars form in dark clouds
More informationGalaxies. CESAR s Booklet
What is a galaxy? Figure 1: A typical galaxy: our Milky Way (artist s impression). (Credit: NASA) A galaxy is a huge collection of stars and interstellar matter isolated in space and bound together by
More informationTHE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES
THE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES DAVID F. GRAY University of Western Ontario, London, Ontario, Canada CAMBRIDGE UNIVERSITY PRESS Contents Preface to the first edition Preface to the
More informationAGB Evolution and Nucleosynthesis at Low-Metallicity Constrained by the Star Formation History of Our Galaxy
AGB Evolution and Nucleosynthesis at Low-Metallicity Constrained by the Star Formation History of Our Galaxy National Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo, 181-8588, Japan E-mail: takuma.suda@nao.ac.jp
More informationCat's Eye Nebula, APOD 4 Sep 02, Corradi & Goncalves. Falk Herwig:»Nuclear Astrophysics with Neutron Facilities«MSU - 14 Feb 05
Cat's Eye Nebula, APOD 4 Sep 02, Corradi & Goncalves Nuclear Astrophysics with Neutron Facilities Falk Herwig Los Alamos National Laboratory, New Mexico, USA Theoretical Astrophysics and Los Alamos Neutron
More informationAge-redshift relation. The time since the big bang depends on the cosmological parameters.
Age-redshift relation The time since the big bang depends on the cosmological parameters. Lyman Break Galaxies High redshift galaxies are red or absent in blue filters because of attenuation from the neutral
More informationarxiv: v1 [astro-ph.sr] 26 Feb 2015
Astronomy & Astrophysics manuscript no. CAbate c ESO 7 September 8, 7 Carbon-enhanced metal-poor stars: a window on AGB nucleosynthesis and binary evolution (I) Detailed analysis of 5 binary stars with
More informationGaia Revue des Exigences préliminaires 1
Gaia Revue des Exigences préliminaires 1 Global top questions 1. Which stars form and have been formed where? - Star formation history of the inner disk - Location and number of spiral arms - Extent of
More information1. The AGB dust budget in nearby galaxies
**Volume Title** ASP Conference Series, Vol. **Volume Number** **Author** c **Copyright Year** Astronomical Society of the Pacific Identifying the chemistry of the dust around AGB stars in nearby galaxies
More informationThe Milky Way. Overview: Number of Stars Mass Shape Size Age Sun s location. First ideas about MW structure. Wide-angle photo of the Milky Way
Figure 70.01 The Milky Way Wide-angle photo of the Milky Way Overview: Number of Stars Mass Shape Size Age Sun s location First ideas about MW structure Figure 70.03 Shapely (~1900): The system of globular
More informationarxiv: v1 [astro-ph.ga] 13 Nov 2012
DRAFT VERSION NOVEMBER 15, 2012 Preprint typeset using LATEX style emulateapj v. 5/2/11 THE MOST METAL-POOR STARS. IV. THE TWO POPULATIONS WITH [FE/H] 3.0 JOHN E. NORRIS 1, DAVID YONG 1, M. S. BESSELL
More informationChapter 7: From theory to observations
Chapter 7: From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, predict the evolution of the stellar bolometric luminosity, effective
More informationStars and their properties: (Chapters 11 and 12)
Stars and their properties: (Chapters 11 and 12) To classify stars we determine the following properties for stars: 1. Distance : Needed to determine how much energy stars produce and radiate away by using
More informationComparison of metal-poor stars in the Milky Way halo and in the dwarf spheroidal galaxy Sculptor, with emphasis on Carbon Enhanced Metal-Poor stars
Comparison of metal-poor stars in the Milky Way halo and in the dwarf spheroidal galaxy Sculptor, with emphasis on Carbon Enhanced Metal-Poor stars Bachelor Research Report Kapteyn Institute Groningen
More informationSignatures of Peculiar Supernova Nucleosynthesis in Extremely α-enhanced Metal-poor Stars
Signatures of Peculiar Supernova Nucleosynthesis in Extremely α-enhanced Metal-poor Stars Hye-Eun Jang 1, Sung-Chul Yoon 1, Young Sun Lee 2, Ho-Gyu Lee 3, Wonseok Kang 4 and Sang-Gak Lee 1 1 Seoul National
More informationNeutron-capture element abundances in the globular clusters: 47 Tuc, NGC 6388, NGC 362 & ω Cen
Neutron-capture element abundances in the globular clusters: 47 Tuc, NGC 6388, NGC 362 & ω Cen C. C. Worley Université de Nice Sophia Antipolis, CNRS (UMR 6202), Observatoire de la Côte d Azur, Cassiopée,
More informationCh. 25 In-Class Notes: Beyond Our Solar System
Ch. 25 In-Class Notes: Beyond Our Solar System ES2a. The solar system is located in an outer edge of the disc-shaped Milky Way galaxy, which spans 100,000 light years. ES2b. Galaxies are made of billions
More informationOxygen in red giants from near-infrared OH lines: 3D effects and first results from. Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto!
Oxygen in red giants from near-infrared OH lines: 3D effects and first results from Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto! Overview! 1. APOGEE: status and prospects! 2. A first look at
More information11/6/18. Today in Our Galaxy (Chap 19)
ASTR 1040: Stars & Galaxies Prof. Juri Toomre TAs: Ryan Horton, Loren Matilsky Lecture 21 Tues 6 Nov 2018 zeus.colorado.edu/astr1040-toomre Edge-on spiral galaxy NGG 4013 Today in Our Galaxy (Chap 19)
More informationLecture 30. The Galactic Center
Lecture 30 History of the Galaxy Populations and Enrichment Galactic Evolution Spiral Arms Galactic Types Apr 5, 2006 Astro 100 Lecture 30 1 The Galactic Center The nature of the center of the Galaxy is
More informationarxiv: v1 [astro-ph.sr] 9 Apr 2013
The elusive origin of Carbon-Enhanced Metal-Poor stars Department of Astrophysics/IMAPP, Radboud Universiteit Nijmegen, Nijmegen, The Netherlands E-mail: C.Abate@astro.ru.nl arxiv:1304.2570v1 [astro-ph.sr]
More informationMilky Way S&G Ch 2. Milky Way in near 1 IR H-W Rixhttp://online.kitp.ucsb.edu/online/galarcheo-c15/rix/
Why study the MW? its "easy" to study: big, bright, close Allows detailed studies of stellar kinematics, stellar evolution. star formation, direct detection of dark matter?? Milky Way S&G Ch 2 Problems
More informationBasics of chemical evolution
Basics of chemical evolution The chemical abundances of stars provide important clues as to the evolutionary history of a galaxy. H and He were present very early on in the Universe, while all metals (except
More informationGalaxies and the Universe. Our Galaxy - The Milky Way The Interstellar Medium
Galaxies and the Universe Our Galaxy - The Milky Way The Interstellar Medium Our view of the Milky Way The Radio Sky COBE Image of our Galaxy The Milky Way Galaxy - The Galaxy By Visual Observation
More informationChapter 8: Simple Stellar Populations
Chapter 8: Simple Stellar Populations Simple Stellar Population consists of stars born at the same time and having the same initial element composition. Stars of different masses follow different evolutionary
More informationFrom theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, give the prediction of the
More informationGalactic Projects at ESO Disk and halo. Birgitta Nordström Niels Bohr Institute Copenhagen University Denmark
Galactic Projects at ESO Disk and halo Birgitta Nordström Niels Bohr Institute Copenhagen University Denmark B. Nordstrom Prague 15 April 2014 1980: Milky Way Structure was Known - the formation and evolution
More informationReport on the new EFOSC2 VPH grisms
Report on the new EFOSC2 VPH grisms Ivo Saviane Lorenzo Monaco v 1.0 March 01, 2008 1 Introduction In January 2008 the ULTRASPEC project delivered two volume-phased holographic grisms (VPHG) to be used
More informationAstr 5465 March 6, 2018 Abundances in Late-type Galaxies Spectra of HII Regions Offer a High-Precision Means for Measuring Abundance (of Gas)
Astr 5465 March 6, 2018 Abundances in Late-type Galaxies Spectra of HII Regions Offer a High-Precision Means for Measuring Abundance (of Gas) Emission lines arise from permitted (recombination) and forbidden
More informationChapter 4. Galactic Chemical Evolution. 4.1 Introduction. 4.2 Chemical Abundances
Chapter 4 Galactic Chemical Evolution 4.1 Introduction Chemical evolution is the term used for the changes in the abundances of the chemical elements in the Universe over time, since the earliest times
More informationThe Milky Way Galaxy. Some thoughts. How big is it? What does it look like? How did it end up this way? What is it made up of?
Some thoughts The Milky Way Galaxy How big is it? What does it look like? How did it end up this way? What is it made up of? Does it change 2 3 4 5 This is not a constant zoom The Milky Way Almost everything
More informationOrigin of Li Anomaly in K giants. Planet engulfment scenario plays role? Bharat Kumar Yerra. Lunch Talk, 22nd October 2014
: Planet engulfment scenario plays role? Stellar Abundances & Galactic Evolution Group NAOC, Beijing Lunch Talk, 22nd October 2014 Collaborators: Dr. B. Eswar Reddy (IIAP, Bangalore, India) Dr. David L.
More informationChapter 19 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Our Galaxy Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition Our Galaxy 19.1 The Milky Way Revealed What does our galaxy look like? How do stars orbit in our galaxy? Where are globular clusters located
More informationPrentice Hall EARTH SCIENCE
Prentice Hall EARTH SCIENCE Tarbuck Lutgens Chapter 25 Beyond Our Solar System 25.1 Properties of Stars Characteristics of Stars A constellation is an apparent group of stars originally named for mythical
More informationRob Izzard. February 21, University of Utrecht. Binary Star Nucleosynthesis. Nucleosynthesis. Single Star Evolution. Binary Star.
University of Utrecht February 21, 2006 Contents Mechanisms Proton capture: H He via pp-chain, CNO, NeNa, MgAl The Sun and most stars Alpha capture: He C, C O, O Ne... Fe Evolved stars C-burning: C + C
More informationThe physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure.
Lecture 4 Stars The physics of stars A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure. X-ray ultraviolet infrared radio To understand
More informationOxygen in AGB stars and the relevance of planetary nebulae to mapping oxygen in the Universe
Oxygen in AGB stars and the relevance of planetary nebulae to mapping oxygen in the Universe Amanda Karakas Research School of Astronomy & Astrophysics Mount Stromlo Observatory, Australia Introduction
More informationLecture 11: Ages and Metalicities from Observations. A Quick Review. Multiple Ages of stars in Omega Cen. Star Formation History.
Ages from main-sequence turn-off stars Lecture 11: Main sequence lifetime: Ages and Metalicities from Observations R diagram lifetime = fuel / burning rate MV *1 M ' L ' MS = 7 10 9 ) ) M. ( L. ( A Quick
More informationLecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4
Lecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4 Key Ideas HR Diagrams of Star Clusters Ages from the Main Sequence Turn-off Open Clusters Young clusters of ~1000 stars Blue Main-Sequence
More informationLecture PowerPoints. Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli
Lecture PowerPoints Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching
More informationFrom theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Update date: December 13, 2010 Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle,
More informationName Date Period. 10. convection zone 11. radiation zone 12. core
240 points CHAPTER 29 STARS SECTION 29.1 The Sun (40 points this page) In your textbook, read about the properties of the Sun and the Sun s atmosphere. Use each of the terms below just once to complete
More informationTopics for Today s Class
Foundations of Astronomy 13e Seeds Chapter 11 Formation of Stars and Structure of Stars Topics for Today s Class 1. Making Stars from the Interstellar Medium 2. Evidence of Star Formation: The Orion Nebula
More informationThree Major Components
The Milky Way Three Major Components Bulge young and old stars Disk young stars located in spiral arms Halo oldest stars and globular clusters Components are chemically, kinematically, and spatially distinct
More informationStellar Populations in the Galaxy
Stellar Populations in the Galaxy Stars are fish in the sea of the galaxy, and like fish they often travel in schools. Star clusters are relatively small groupings, the true schools are stellar populations.
More informationAstronomy 242: Review Questions #3 Distributed: April 29, 2016
Astronomy 242: Review Questions #3 Distributed: April 29, 2016 Review the questions below, and be prepared to discuss them in class next week. Modified versions of some of these questions will be used
More informationLearning Objectives: Chapter 13, Part 1: Lower Main Sequence Stars. AST 2010: Chapter 13. AST 2010 Descriptive Astronomy
Chapter 13, Part 1: Lower Main Sequence Stars Define red dwarf, and describe the internal dynamics and later evolution of these low-mass stars. Appreciate the time scale of late-stage stellar evolution
More information18. Stellar Birth. Initiation of Star Formation. The Orion Nebula: A Close-Up View. Interstellar Gas & Dust in Our Galaxy
18. Stellar Birth Star observations & theories aid understanding Interstellar gas & dust in our galaxy Protostars form in cold, dark nebulae Protostars evolve into main-sequence stars Protostars both gain
More informationThe Stars. Chapter 14
The Stars Chapter 14 Great Idea: The Sun and other stars use nuclear fusion reactions to convert mass into energy. Eventually, when a star s nuclear fuel is depleted, the star must burn out. Chapter Outline
More informationUniversity of Naples Federico II, Academic Year Istituzioni di Astrofisica, read by prof. Massimo Capaccioli. Lecture 16
University of Naples Federico II, Academic Year 2011-2012 Istituzioni di Astrofisica, read by prof. Massimo Capaccioli Lecture 16 Stellar populations Walter Baade (1893-1960) Learning outcomes The student
More informationThe Milky Way Galaxy (ch. 23)
The Milky Way Galaxy (ch. 23) [Exceptions: We won t discuss sec. 23.7 (Galactic Center) much in class, but read it there will probably be a question or a few on it. In following lecture outline, numbers
More informationSubstructure in the Galaxy
Substructure in the Galaxy Amina Helmi Kapteyn Astronomical Institute Groningen, NL Is this how our Galaxy formed? Jeffrey Gardner Hierarchical paradigm Main characteristic of model: mergers Can we find
More informationMapping the oxygen abundance in an elliptical galaxy (NGC 5128)
Mapping the oxygen abundance in an elliptical galaxy (NGC 5128) Jeremy R. Walsh, ESO Collaborators: George H. Jacoby, GMT Observatory, Carnegie; Reynier Peletier, Kapteyn Lab., Groningen; Nicholas A. Walton,
More informationStudying stars in M31 GCs using NIRI and GNIRS
Studying stars in M31 GCs using NIRI and GNIRS Ricardo Schiavon Gemini Observatory GSM 2012 San Francisco July 19, 2012 Collaborators Andy Stephens (Gemini) Nelson Caldwell (SAO) Matthew Shetrone (HET)
More informationChapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
More informationMar 22, INSTRUCTIONS: First ll in your name and social security number (both by printing
ASTRONOMY 0089: EXAM 2 Class Meets M,W,F, 1:00 PM Mar 22, 1996 INSTRUCTIONS: First ll in your name and social security number (both by printing and by darkening the correct circles). Sign your answer sheet
More informationGamma-Ray Astronomy. Astro 129: Chapter 1a
Gamma-Ray Bursts Gamma-Ray Astronomy Gamma rays are photons with energies > 100 kev and are produced by sub-atomic particle interactions. They are absorbed by our atmosphere making observations from satellites
More informationOxygen in the Early Galaxy: OH Lines as Tracers of Oxygen Abundance in Extremely Metal-Poor Giant Stars
Oxygen in the Early Galaxy: OH Lines as Tracers of Oxygen Abundance in Extremely Metal-Poor Giant Stars A. Kučinskas 1, V. Dobrovolskas 1, P. Bonifacio 2, E. Caffau 2, H.-G. Ludwig 3, M. Steffen 4, M.
More informationA Zoo of Ancient Stellar Relics in our Galactic Halo
A Zoo of Ancient Stellar Relics in our Galactic Halo Simon W. Campbell1,2 1) GAA, Dept. Fisica i Enginyeria Nuclear, Universitat Politecnica de Catalunya 2) CSPA, Australia (Centre for Stellar and Planetary
More informationchapter 31 Stars and Galaxies
chapter 31 Stars and Galaxies Day 1:Technology and the Big Bang Studying the Stars A. Telescopes - Electromagnetic radiation emitted by stars and other objects include light, radio, and X-ray Space telescopes
More informationStellar Evolution. Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars
Lecture 11 Stellar Evolution Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars A Spiral Galaxy (Milky Way Type) 120,000 ly A few hundred billion stars
More informationAstronomy 1144 Exam 3 Review
Stars and Stellar Classification Astronomy 1144 Exam 3 Review Prof. Pradhan 1. What is a star s energy source, or how do stars shine? Stars shine by fusing light elements into heavier ones. During fusion,
More informationHigh resolution spectroscopy of two metal-poor red giants: HD and HD
High resolution spectroscopy of two metal-poor red giants: HD 3078 and HD 1873 Faculty of Physics and Mathematics, University of Latvia, Raiņa bulv. 19, Riga, LV-1586, Latvia E-mail: arturs_ lv@inbox.lv
More informationPaul Broberg Ast 4001 Dec. 10, 2007
Paul Broberg Ast 4001 Dec. 10, 2007 What are W-R stars? How do we characterize them? What is the life of these stars like? Early stages Evolution Death What can we learn from them? Spectra Dust 1867: Charles
More informationNucleosynthesis in heliumenriched
Nucleosynthesis in heliumenriched stars Amanda Karakas With Anna Marino and David Nataf Outline 1. The effect of helium enrichment on the evolution and nucleosynthesis of lowmetallicity AGB models 2. The
More informationLate Stages of Stellar Evolution. Late Stages of Stellar Evolution
Late Stages of Stellar Evolution The star enters the Asymptotic Giant Branch with an active helium shell burning and an almost dormant hydrogen shell Again the stars size and luminosity increase, leading
More information