NGC 6273

Evidence for Enrichment by Supernovae in the Globular Cluster NGC 6273

Sang-Il Han11affiliation: Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 03722, Korea 22affiliation: Korea Astronomy and Space Science Institute, Daejeon 34055, Korea 33affiliation: Both authors have contributed equally to this paper. , Dongwook Lim11affiliation: Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 03722, Korea 33affiliation: Both authors have contributed equally to this paper. , Hyunju Seo11affiliation: Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 03722, Korea , Young-Wook Lee11affiliation: Center for Galaxy Evolution Research and Department of Astronomy, Yonsei University, Seoul 03722, Korea 44affiliation: Corresponding author: ywlee2@yonsei.ac.kr
Abstract

In our recent investigation (Lim et al., 2015), we have shown that narrow-band photometry can be combined with low-resolution spectroscopy to effectively search for globular clusters (GCs) with supernovae (SNe) enrichments. Here we apply this technique to the metal-poor bulge GC NGC 6273, and find that the red giant branch stars in this GC are clearly divided into two distinct subpopulations having different calcium abundances. The Ca rich subpopulation in this GC is also enhanced in CN and CH, showing a positive correlation between them. This trend is identical to the result we found in M22, suggesting that this might be a ubiquitous nature of GCs more strongly affected by SNe in their chemical evolution. Our results suggest that NGC 6273 was massive enough to retain SNe ejecta which would place this cluster in the growing group of GCs with Galactic building block characteristics, such as  Centauri and Terzan 5.

Subject headings:
Galaxy: formation — globular clusters: general — globular clusters: individual (NGC 6273) — stars: abundances — stars: evolution

1. Introduction

One of the problems of the CDM hierarchical merging paradigm in local scale is that the observed number of the remaining “building blocks” in the Milky Way is about an order of magnitude smaller than the predicted number of subhalos (see, e.g., Kauffmann et al., 1993; Moore et al., 2006). Despite the recent progress in searching for the ultra faint dwarf galaxies (e.g., Willman et al., 2005; Zucker et al., 2006; Belokurov et al., 2007; Bechtol et al., 2015, references therein), this “missing satellite problem” still requires additional search for the building block candidates in the Milky Way. Not well known to the community is a possibility that some massive globular clusters (GCs) might be originated from proto-galactic subsystems (Searle & Zinn, 1978; Freeman, 1993). Starting from  Centauri (Lee et al., 1999; Bedin et al., 2004), increasing number of GCs now show evidence of supernovae (SNe) enrichment, indicating that their original mass was heavy enough to retain SNe ejecta (Dopita & Smith, 1986; Baumgardt et al., 2008), which would place them as remaining nuclei of disrupted dwarf galaxies. As of August 2015, GCs belong to this category include  Cen (Lee et al., 1999; Bedin et al., 2004), M54 (Siegel et al., 2007), M22 (J.-W. Lee et al., 2009; Da Costa et al., 2009; Marino et al., 2009), Terzan 5 (Ferraro et al., 2009), NGC 1851 (J.-W. Lee et al., 2009; Han et al., 2009; Carretta et al., 2010b), NGC 2419 (Cohen & Kirby, 2012; Mucciarelli et al., 2012; Lee et al., 2013), NGC 5824 (Da Costa et al., 2014), M2 (Yong et al., 2014), and NGC 5286 (Marino et al., 2015). Although it is widely accepted by the community that almost all GCs were initially much more massive (e.g., Decressin et al., 2007; D’Ercole et al., 2008; Carretta et al., 2010a; Conroy & Spergel, 2011; Schaerer & Charbonnel, 2011), these GCs that were able to retain SNe ejecta were probably even more massive (M 10M; Decressin et al., 2010), and therefore, could have provided more stars to halo field.

More massive GCs in the Milky Way bulge are expected to have this characteristic (Diemand et al., 2007; Lee et al., 2007; Ferraro et al., 2009; Lim et al., 2015). Detailed studies for these GCs, however, are hampered by highly obscured environment in which they are placed. The near IR photometry and spectroscopy would be ideal probes to detect any evidence for multiple populations in these GCs as shown, for example, by Ferraro et al. (2009) for the case of Terzan 5. As suggested by Lim et al. (2015, hereafter Paper I), in the case of mildly obscured GCs in the bulge, however, the combination of narrow-band Ca photometry and low-resolution spectroscopy can effectively disentangle the reddening and metallicity effects. The purpose of this letter is to report our discovery, by employing this technique, that NGC 6273 also belongs to this growing body of GCs.

Figure 1.— CMDs for NGC 6273 in () and () planes. The top panels show all stars while the middle panels are for stars within 3. The horizontal bars denote the measurement error (1). Spectroscopic targets are identified on the bottom panels, where blue and red circles denote stars selected from the bluer and redder RGBs, respectively.
Figure 2.— Measured HK (upper panels) and CN (lower panels) indices as functions of magnitude. The HK and CN indices in the right panels are obtained from the height of the HK and CN indices above the least-square lines in the left panels. The blue and red circles are stars in bluer and redder RGBs in the bottom panels of Figure 1. The solid and dashed lines indicate the mean value and the standard deviation of the mean (1) for each subpopulation, respectively. The vertical bars in the right panels show the typical measurement error for HK and CN indices. (Supplemental data for this figure are available in the online journal.)

2. Presence of two red giant branches with different Ca abundances

Our observations, both narrow-band Ca photometry and low-resolution spectroscopy, were made on the du Pont 2.5m telescope at Las Campanas Observatory during the 14 nights from 2011 to 2014. The narrow-band Ca photometry covered 15′ 15′ field centered on the cluster. Total exposure times for the central region (9′ 9′) were 12600, 2520, and 1260 sec for Ca, , and filters, respectively, and those for the outer regions were 3600, 720, and 360 sec. The low-resolution spectroscopy was performed on the multi-object spectroscopic mode of the Wide Field Reimaging CCD (WFCCD) in the same field covered by the photometry. The exposure times were between 1200 and 1800 sec, depending on the magnitude of the target stars in the masks. For the data reduction, both for the photometry and spectroscopy, we followed the same manner described in Paper I – IRAF111IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. for the preprocessing, DAOPHOT II/ALLSTAR and ALLFRAME (Stetson, 1987, 1994) for the point spread function photometry, and the modified WFCCD reduction package (Prochaska et al. 2006; Paper I) for the spectroscopic analysis. Readers are referred to Paper I for the details of procedures adopted in our data reduction.

Figure 1 shows color-magnitude diagrams (CMDs) for NGC 6273 in () and () planes, where the index is defined as Ca (Anthony-Twarog et al., 1991). As described in Paper I, stars affected by adjacent starlight contamination and bad measurements were rejected (i.e., 0.5, 1.5, and SHARP ). We adopted more rigorous criterion as to the index (less than 0.5 instead of 1.0 as adopted in Paper I) because of a larger field star contamination in the bulge field where NGC 6273 is placed. The top panels of Figure 1 show all stars in our program field, where the field star contamination (mostly main-sequence stars in the disk and red giant branch stars in the bulge) is evident. The stars within 3′ from the cluster center are shown in the middle panels where the CMD features from the cluster members are more clearly visible. In these panels, the most notable feature is the presence of two distinct red giant branch (RGB) subpopulations in the () CMD, while this split is not apparent in the () CMD, suggesting a difference in calcium abundance between the two RGB sequences. Note that this spilt is also present on the sub giant branch in the () CMD. The difference in the index between the two RGBs is about 0.12 mag at the magnitude level of the horizontal-branch. While some field star contamination is still present222Photometry for a control field obtained in the same observing run which is two tidal radius away from the cluster center shows field star contamination is small (less than 6%) in the regime occupied by two RGBs in the mag range of 16 17., the population ratio between the bluer and redder RGBs, defined by the difference in from the fiducial line ( 0.06 for bluer RGB, 0.06 for redder RGB), is estimated to be 0.6:0.4 for the stars in the mag range of 16 17.

In order to confirm the difference in calcium abundance between the two RGBs, we have measured spectroscopic HK, HK, CN, and CN indices defined in Paper I for a similar number of stars selected from each RGB. The target stars are shown in the bottom panels of Figure 1, and Figure 2 shows measured indices as functions of magnitude. The right panels of Figure 2 are the differences in HK and CN indices (HK and CN) measured from the least-square fits (black solid lines in left panels) to show only the abundance effect at fixed temperature and gravity (see Paper I). The mean differences in HK and CN indices between the two subpopulations are 0.05 dex and 0.31 dex, respectively, in the sense that the redder RGB stars are more enhanced. These differences are significant at 6.3 level for HK and at 6.4 level for CN compared to the standard deviation of the mean for each group.

Figure 3.— Measured HK index as a function of color. The blue and red solid lines are the least-square lines for each subpopulation, respectively. The red dashed line indicates the expected locus of redder RGB stars if the RGB split is due to the reddening.

Since some differential reddening is reported in the field toward NGC 6273 (0.2; Piotto et al. 1999), it is important to check whether the RGB split is affected by the reddening. In order to examine this, we plot HK index versus color in Figure 3. If the RGB split is due to the reddening, the redder RGB stars would be placed on the right side in this diagram or around the red dashed line. However, the observed redder RGB stars are located in the opposite regime as would be expected if they are enhanced in HK. This confirms, together with the discrete distribution of the two RGB sequences on the CMD, that the effect from the differential reddening, if any, is not significant. Furthermore, note that the index has a little dependence on the reddening, and (Anthony-Twarog et al., 1991; J.-W. Lee et al., 2009).

Figure 4.— Difference in metallicity between the two RGB subpopulations in NGC 6273. Blue and red circles denote bluer and redder RGB stars, respectively, for which cross-matched spectroscopic data are available in Johnson et al. (2015, filled circles) and Rutledge et al. (1997, open circles). The redder RGB stars are enhanced in [Fe/H] and [Ca/H] (see panels (b) and (c)). The index in panels (b)-(d) is defined as the difference from the fiducial line (green solid line in panel (a)). The solid and dashed lines indicate, respectively, the mean value and 1 error of the mean for each subpopulation.

3. Discussion

We have shown that the RGB stars in NGC 6273 are divided into two distinct subgroups in the narrow-band Ca photometry. Our low-resolution spectroscopy confirms that the origin of this split is indeed due to the difference in calcium abundance between the two RGBs. After the draft of this paper was completed, the iron spread in this GC was recently reported by Johnson et al. (2015) from high-resolution spectroscopy of 18 RGB stars. While this result is qualitatively consistent with our finding, the discrete nature of the metallicity distribution function is more clearly shown in this investigation from the narrow-band Ca photometry for 1,600 RGB stars, together with the low-resolution spectroscopy for 78 stars.

In order to see whether the calcium enhanced stars in our sample are similarly enhanced in iron abundance, in panel (a) of Figure 4, we have cross-matched stars in Johnson et al. (2015) with those in our sample (filled circles). The two subpopulations were defined from the photometry by the difference in from the fiducial line as described in Section 2. Panel (b) shows that the calcium enhanced stars in our observations are enhanced in [Fe/H] as well, with the difference of 0.2 dex (4.0 level). Calcium abundance obtained from Johnson et al. (2015) in panel (c) also confirms the difference in [Ca/H] (0.24 dex, 4.4 level).333The two subpopulations also appear to show the difference in [Mg/Fe]. However, when [Mg/H] is plotted, instead of [Mg/Fe], we found no difference between the two groups as correctly pointed out by the referee. This confirms that the apparent difference in [Mg/Fe] is only the reflex of the variation in Fe between the two subpopulations. We also compare the Ca II triplet measurements of Rutledge et al. (1997) with our photometry (open circles), where the difference in [Ca/H] was deduced from their reduced equivalent widths (Ca). In this case, the mean difference in [Ca/H] between the two subpopulations is 0.16 dex, which is significant at 9.3 level (see panel (d)).

Figure 5.— The correlation between CN and CH indices. The RGB stars in NGC 6273 show a positive correlation, which is qualitatively similar to the case of M22. The dashed line is a least-square fit.

Figure 5 presents the correlation between CN and CH for the RGB stars in NGC 6273, which shows a positive correlation. As discussed in Paper I (see Figure 13), most “normal” GCs show anti-correlation between CN and CH, while some massive GCs enriched by SNe, such as M22, show positive correlation. It was suggested in Paper I that this systematic difference would reflect how strongly SNe have enriched the later generation of stars. The fact that NGC 6273 is following the same trend observed in M22 is also consistent with our conclusion that the chemical evolution in this GC was relatively strongly affected by SNe. This further suggests that NGC 6273 was massive enough to retain SNe ejecta, which would place this cluster in the growing group of GCs with Galactic building block origin, such as  Cen and Terzan 5. In particular, this places NGC 6273 as the first metal-poor ([Fe/H] -1.5) GC in the bulge field with this characteristic.

We are indebted to the anonymous referee for a number of helpful suggestions which led to several improvements in the manuscript. We also thank the staff of LCO for their support during the observations. Support for this work was provided by the National Research Foundation of Korea to the Center for Galaxy Evolution Research and by the Korea Astronomy and Space Science Institute under the R&D program (No. 2014-1-600-05) supervised by the Ministry of Science, ICT and future Planning.

References

  • Anthony-Twarog et al. (1991) Anthony-Twarog, B. J., Laird, J. B., Payne, D., & Twarog, B. A. 1991, AJ, 101, 1902
  • Baumgardt et al. (2008) Baumgardt, H., Kroupa, P., & Parmentier, G. 2008, MNRAS, 384, 1231
  • Bechtol et al. (2015) Bechtol, K., Drlica-Wagner, A., Balbinot, E., et al. 2015, ApJ, 807, 50
  • Bedin et al. (2004) Bedin, L. R., Piotto, G., Anderson, J., et al. 2004, ApJ, 605, L125
  • Belokurov et al. (2007) Belokurov, V., Zucker, D. B., Evans, N. W., et al. 2007, ApJ, 654, 897
  • Carretta et al. (2010a) Carretta, E., Bragaglia, A., Gratton, R. G., et al. 2010a, A&A, 516, 55
  • Carretta et al. (2010b) Carretta, E., Gratton, R. G., Lucatello, S., et al. 2010b, ApJ, 722, L1
  • Cohen & Kirby (2012) Cohen, J. G., & Kirby, E. N. 2012, ApJ, 760, 86
  • Conroy & Spergel (2011) Conroy, C., & Spergel, D. N. 2011, ApJ, 726, 36
  • Da Costa et al. (2009) Da Costa, G. S., Held, E. V., Saviane, I., & Gullieuszik, M. 2009, ApJ, 705, 1481
  • Da Costa et al. (2014) Da Costa, G. S., Held, E. V., & Saviane, I. 2014, MNRAS, 438, 3507
  • Decressin et al. (2007) Decressin, T., Meynet, G., Charbonnel, C., Prantzos, N., & Ekstrom, S. 2007, A&A, 464, 1029
  • Decressin et al. (2010) Decressin, T., Baumgardt, H., Charbonnel, C., & Kroupa, P. 2010, A&A, 516, A73
  • D’Ercole et al. (2008) D’Ercole, A., Vesperini, E., D’Antona, F., McMillan, S. L. W., & Recchi, S. 2008, MNRAS, 391, 825
  • Diemand et al. (2007) Diemand, J., Kuhlen, M., & Madau, P. 2007, ApJ, 667, 859
  • Dopita & Smith (1986) Dopita, M. A., & Smith, G. H. 1986, ApJ, 304, 283
  • Ferraro et al. (2009) Ferraro, F. R., Dalessandro, E., Mucciarelli, A., et al. 2009, Nature, 462, 483
  • Freeman (1993) Freeman, K. C. 1993, in ASP Conf. Ser. 48, The Globular Clusters-Galaxy Connection, ed. G. H. Smith & J. P. Brodie (San Francisco: ASP), 608
  • Han et al. (2009) Han, S.-I., Lee, Y.-W., Joo, S.-J., et al. 2009, ApJ, 707, L190
  • Johnson et al. (2015) Johnson, C. I., Rich, M., Pilachowski, C. A., et al. 2015, AJ, 150, 63
  • Kauffmann et al. (1993) Kauffmann, G., White, S. D. M., & Guiderdoni, B. 1993, MNRAS, 264, 201
  • J.-W. Lee et al. (2009) Lee, J.-W., Kang, Y.-W., Lee, J., & Lee, Y.-W. 2009, Nature, 462, 480
  • Lee et al. (1999) Lee, Y.-W., Joo, J.-M., Sohn, Y.-J., et al. 1999, Nature, 402, 55
  • Lee et al. (2007) Lee, Y.-W., Gim, H. B., & Casetti-Dinescu, D. I. 2007, ApJ, 661, L49
  • Lee et al. (2013) Lee, Y.-W., Han, S.-I., Joo, S.-J., et al. 2013, ApJ, 778, L13
  • Lim et al. (2015) Lim, D., Han, S.-I., Lee, Y.-W., et al. 2015, ApJS, 216, 19
  • Marino et al. (2009) Marino, A. F., Milone, A. P., Piotto, G., et al. 2009, A&A 505, 1099
  • Marino et al. (2015) Marino, A. F., Milone, A. P., Karakas, A. I., et al. 2015, MNRAS, 450, 815
  • Moore et al. (2006) Moore, B., Diemand, J., Madau, P., Zemp, M., & Stadel, J. 2006, MNRAS, 368, 563
  • Mucciarelli et al. (2012) Mucciarelli, A., Bellazzini, M., Ibata, R., Merle, T., & Chapman, S. C. 2012, MNRAS, 426, 2889
  • Prochaska et al. (2006) Prochaska, J. X., Weiner, B. J., Chen, H.-W., & Mulchaey, J. S. 2006, ApJ, 643, 680
  • Piotto et al. (1999) Piotto, G., Zoccali, M., King, I. R., et al. 1999, AJ, 118, 1727
  • Rutledge et al. (1997) Rutledge, G. A., Hesser, J. E., Stetson, P. B., et al. 1997, PASP, 109, 883
  • Schaerer & Charbonnel (2011) Schaerer, D., & Charbonnel, C. 2011, MNRAS, 413, 2297
  • Searle & Zinn (1978) Searle, L. & Zinn, R. 1978, ApJ, 225, 357
  • Siegel et al. (2007) Siegel, M. H., Dotter, A., Majewski, S. R., et al. 2007, ApJ, 667, L57
  • Stetson (1987) Stetson, P. B. 1987, PASP, 99, 191
  • Stetson (1994) Stetson, P. B. 1994, PASP, 106, 250
  • Willman et al. (2005) Willman, B., Blanton, M. R., West, A. A., et al. 2005, AJ, 129, 2692
  • Yong et al. (2014) Yong, D., Roederer, I. U., Grundahl, F., et al. 2014, MNRAS, 441, 3396
  • Zucker et al. (2006) Zucker, D. B., Belokurov, V., Evans, N. W., et al. 2006, ApJ, 643, L103
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
321469
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description