Contents

A&A 417, 293-300 (2004)
DOI: 10.1051/0004-6361:20031759

Chemical composition of UV-bright star ZNG 4 in the globular cluster M 13[*],[*]

S. Ambika 1 - M. Parthasarathy 1 - W. Aoki 2 - T. Fujii 2,3 - Y. Nakada 4,5 - Y. Ita 4 - H. Izumiura 6


1 - Indian Institute of Astrophysics, Koramangala, Bangalore, 560034, India
2 - National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
3 - Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima 890-0065, Japan
4 - Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo, 181-0015, Japan
5 - Kiso Observatory, Institute of Astronomy, University of Tokyo, Mitake, Kiso, Nagano 397-0101, Japan
6 - Okayama Astrophysical Observatory, National Astronomical Observatory, Kamogata, Okayama 719-0232, Japan

Received 20 May 2003 / Accepted 18 November 2003

Abstract
We present a detailed model-atmosphere analysis of ZNG 4, a UV-bright star in the globular cluster M 13. From the analysis of a high resolution ( $ R \approx 45~000 $) spectrum of the object, we derive the atmospheric parameters to be $T_{\rm eff} = 8500\pm 250$ K, log  $g = 2.5 \pm 0.5$ and $\rm [Fe/H]= -1.5$. Except for magnesium, chromium and strontium, all other even Z elements are enhanced with titanium and calcium being overabundant by a factor of 0.8 dex. Sodium is enhanced by a factor of 0.2 dex. The luminosity of ZNG 4 and its position in the color-magnitude diagram of the cluster indicate that it is a Supra Horizontal Branch (SHB) (post-HB) star. The underabundance of He and overabundances of Ca, Ti, Sc and Ba in the photosphere of ZNG 4 indicate that diffusion and radiative levitation of elements may be in operation in M 13 post-HB stars even at $T_{\rm eff}$ of 8500 K. Detailed and more accurate abundance analysis of post-HB stars in several globular clusters is needed to further understand their abundance anomalies.

Key words: stars: abundances - stars: evolution - stars: Population II - stars: horizontal-branch - Galaxy: globular cluster: individual: M 13 - stars: individual: ZNG 4

1 Introduction

The term "UV-bright stars" was introduced by Zinn et al. (1972) for stars in globular clusters that lie above the horizontal branch (HB) and are bluer than red giants. The name resulted from the fact that, in the U band, these stars were brighter than all other cluster stars. Further investigations showed that this group of stars consist of blue horizontal branch (BHB) stars, supra horizontal branch stars (SHB), post asymptotic giant branch stars (post-AGB), post-early AGB (P-EAGB) stars and AGB-manque stars (de Boer 1985, 1987; Sweigart et al. 1974; Brocato et al. 1990; Dorman et al. 1993; Gonzalez & Wallerstein 1994).

To derive the chemical composition of UV-bright stars in globular clusters and to understand their evolutionary stages, we started a program to obtain high resolution spectra of these objects in selected globular clusters with the High Dispersion Spectrograph (HDS, Noguchi et al. 2002) of the 8.2 m Subaru Telescope. We selected a few UV-bright stars in the globular cluster M 13 from the papers of Zinn et al. (1972) and Harris et al. (1983) to derive their chemical composition. In this paper we report the analysis of a high resolution spectrum of the UV-bright star ZNG 4 (RA ( $16^{\rm h}41^{\rm m}37\hbox{$.\!\!^{\rm s}$ }528$) and Dec ( $+36\degr30\hbox{$^\prime$ }43.86\hbox{$^{\prime\prime}$ }$) (2000)) (Zinn et al. 1972) in M 13 as the first target of our program.

M 13 (NGC 6205) is a nearby wellstudied globular cluster with a distance modulus of $(m-M)_0 = 14\hbox{$.\!\!^{\rm m}$ }42$ and metallicity of $\rm [Fe/H] = -1.51$ (Kraft & Ivans 2003). The position of ZNG 4 in the color-magnitude diagram of M 13 (Paltrinieri et al. 1998) is shown in Fig. 1. Many of the globular clusters show a prominent gap in the blue tail of the HB, which is presumed to be due to differential mass loss on the Red Giant Branch (RGB). In M 13 it is observed at $T_{\rm eff} = 10~000$ K (Ferraro et al. 1997). High resolution spectroscopic studies of M 13 BHB stars lying on either side of the gap were carried out by Peterson et al. (1983, 1995) and Behr et al. (1999, 2000a). They found anomalous photospheric abundances in BHB stars. These photospheric anomalies are most likely due to diffusion - the gravitational settling of helium and radiative levitation of the metal atoms in the stable atmosphere of hot stars. They found variations in the photospheric abundances and rotational velocities of BHB stars as a function of their effective temperatures.


  \begin{figure}
\par\includegraphics[width=8.5cm,clip]{star2.eps}\end{figure} Figure 1: Color magnitude diagram (CMD) of globular cluster M 13 obtained by Paltrinieri et al. (1998). The arrow indicates the position of ZNG 4 in the CMD.

2 Observations

We have obtained a high resolution ( $\rm\frac {\lambda} {\Delta \lambda}
\approx 45~000$) spectrum of ZNG 4 on 15th (UT: 14h 45m) April 2001 with the Subaru/HDS. The spectrum covering the wavelength range 4142 $\AA$-6814 $\AA$ was obtained in an exposure time of 20 min. There was no moon light problem during the observations and the sky background in the data was close to zero. We neglected the sky background in our data reduction.

The data was bias-subtracted, trimmed, flat-fielded to remove pixel to pixel variations, converted to a one-dimensional spectrum, and normalized to the continuum using standard CCD data reduction package (NOAO IRAF). The spectrum has an average signal to noise ratio of 35. The reference spectrum of thorium-argon was used for the wavelength calibration.

The various orders in our echelle spectrum of ZNG 4 have well defined continuum and the normalization of the continuum was carried out using the IRAF echelle spectra reduction programs. The continuum level in the adjacent echelle orders to those containing the Balmer lines was useful in defining the continuum in the Balmer line regions and the profiles were normalized with a polynomial fit.

3 Analysis

The spectral lines were identified using Moore's atomic multiplet table (1945). Equivalent widths of the absorption lines were measured using the routines available in the SPLOT package of IRAF. The equivalent widths were measured by Gaussian fitting to the observed profiles (and a multiple Gaussian fit to the blended lines such as the Mg II lines at 4481 $\AA$) and are given in Table 3.

3.1 Radial velocity

The radial velocity of ZNG 4 was derived from the wavelength shifts of many absorption lines. The average heliocentric velocity is found to be $V\rm _r = -257.56 \pm 1.08$ $\rm km$  $\rm s^{-1}$ which is in agreement with the value derived by Zinn (1974) (-253 km s-1). It is also in agreement with the heliocentric velocities of M 13 BHB stars derived by Behr et al. (1999) and Moehler et al. (2003).

3.2 Atmospheric parameters

For the initial estimate of effective temperature, we looked for the published CCD photometry of the star. Recent CCD photometry of M 13 was carried out by Rey et al. (2001). However the ZNG 4 area of the cluster was not included in their observations (Rey, private communication). We used the published CCD photometry of ZNG 4 by Paltrinieri et al. (1998), who give, B=14.096 and V=13.964. (B-V) = 0.132 and E(B-V) = 0.02 (Kraft & Ivans 2003) will yield (B-V)0 = 0.112 which corresponds to $T_{\rm eff} = 8373$ K (Flower 1996). However, the (B-V)0 and $T_{\rm eff}$ calibration given by Flower (1996) is for Population I stars.

For our analysis, excitation potential and oscillator strengths of the lines were taken from the Vienna Atomic Line Database (http://www.astro.univie.ac.at/~vald/). We employed the latest (2002) version of MOOG, an LTE stellar line analysis program (Sneden 1973) and Kurucz (1993) grid of ATLAS models. MOOG has been used successfully in the analysis of the spectra of warmer stars with $T_{\rm eff} = 7900$ K (Preston & Sneden 2000).

We have also analyzed the spectra using the Kurucz WIDTH program (Kurucz CDROM 13, 1993) for verification. We used the line list obtained using version 43 of the Synspec code of Hubeny and Lanz which is distributed as part of their TLUSTY model atmosphere program. (http://tlusty.gsfc.nasa.gov/Synspec43/synspec-line.html) and also the information from the Kurucz linelist (http://kurucz.harvard.edu/linelists.html).

The value of effective temperature was obtained by the method of excitation balance, forcing the slope of abundances from Fe I lines versus excitation potential to be zero. The surface gravity was then set by ionization- equilibrium, forcing abundances obtained from neutral (Fe I) and ionized (Fe II) species to be equal. The microturbulent velocity was estimated by demanding that there should be no dependence of the Fe I abundance upon equivalent widths of Fe I lines.


  \begin{figure}
\par\includegraphics[angle=90,width=12.5cm,clip]{fech1.eps}\par\end{figure} Figure 2: Top figure is the plot of the abundances from Fe lines versus excitation potential of the lines. Figure at the bottom is the plot of the abundances from Fe lines versus their equivalent widths. Triangles represent the Fe I lines and stars denote the Fe II lines.

The plots of the abundances versus excitation potentials and abundances versus equivalent widths in the case of Fe I and Fe II lines are shown in Fig. 2. Such plots were made by varying the $T_{\rm eff}$, log gand $V_{\rm t}$ in steps of 250 K, 0.5 and 0.5 km  $\rm s^{-1}$ respectively to estimate the uncertainties in these parameters.

From our analysis, we find that $T_{\rm eff} = 8500$ K, log g = 2.5 and $V_{\rm t}=2.5~\rm km~s^{-1}$ fit the data best (Fig. 2). From the abovementioned method of analysis we find the uncertainties in $T_{\rm eff}$to be 250 K, log g = 0.5 dex and $V_{\rm t}= 0.5$ km  $\rm s^{-1}$. Uncertainties in derived abundances as a result of errors in the determination of the parameters and errors in the measurements of equivalent widths are found to be of the order of 0.2 dex.


 

 
Table 1: Chemical composition of ZNG 4 in M 13.

Element

No. of lines $T_{\rm eff} = 8500$ K, log g= 2.5 $T_{\rm eff} = 8500$ K, log g= 2.5 $T_{\rm eff} = 8750$ K, log g= 2.0
    $V_{\rm t} = 2$ km  $\rm s^{-1}$ and $V_{\rm t} = 2$ km  $\rm s^{-1}$ and $V_{\rm t} = 2$ km  $\rm s^{-1}$ and
    $\rm [Fe/H]= -1.5$ $\rm [Fe/H]= -1.5$ $\rm [Fe/H]= -1.5$
    MOOG WIDTH MOOG
    $ \rm [X/H] \pm \sigma $ [Ele/Fe] $ \rm [X/H] \pm \sigma $ [ Ele/Fe] $ \rm [X/H] \pm \sigma $

He I

1 -0.55 $\pm$ 0.20   -0.68 $\pm$ 0.20   -1.13 $\pm$ 0.31
Na I 2 -1.28 $\pm$ 0.10 +0.21 -1.30 $\pm$ 0.10 +0.20 -0.79 $\pm$ 0.11
Mg I 3 -1.46 $\pm$ 0.07 +0.03 -1.48 $\pm$ 0.05 +0.02 -1.03 $\pm$ 0.16
Mg II 2 -1.56 $\pm$ 0.14 -0.07 -1.59 $\pm$ 0.09 -0.09 -1.83 $\pm$ 0.15
Si II 4 -1.10 $\pm$ 0.15 +0.39 -1.20 $\pm$ 0.12 +0.30 -1.31 $\pm$ 0.24
Ca I 2 -0.80 $\pm$ 0.35 +0.69 -0.93 $\pm$ 0.25 +0.57 -0.09 $\pm$ 0.33
Ca II 1 -0.49 $\pm$ 0.10 +1.00 -0.62 $\pm$ 0.10 +0.88 -0.32 $\pm$ 0.10
Sc II 7 -0.99 $\pm$ 0.25 +0.50 -1.04 $\pm$ 0.25 +0.45 -0.73 $\pm$ 0.25
Ti II 51 -0.75 $\pm$ 0.18 +0.74 -0.83 $\pm$ 0.25 +0.67 -0.59 $\pm$ 0.19
Cr II 8 -1.41 $\pm$ 0.12 +0.08 -1.47 $\pm$ 0.12 +0.03 -1.38 $\pm$ 0.12
Fe I 13 -1.48 $\pm$ 0.15 +0.02 -1.53 $\pm$ 0.26 +0.02 -0.99 $\pm$ 0.14
Fe II 28 -1.50 $\pm$ 0.21 +0.00 -1.46 $\pm$ 0.22 +0.02 -1.52 $\pm$ 0.22
Sr II 1 -2.19 $\pm$ 0.10 -0.70 -2.21 $\pm$ 0.10 -0.71 -1.65 $\pm$ 0.12
Y II 2 -1.20 $\pm$ 0.17 +0.29 -1.30 $\pm$ 0.12 +0.37 -0.64 $\pm$ 0.14
Ba II 2 -1.21 $\pm$ 0.05 +0.28 -1.23 $\pm$ 0.04 +0.26 -0.61 $\pm$ 0.10


Using the derived atmospheric parameters and abundances, a synthetic spectrum was generated and plotted over the observed spectrum for verification. The observed and synthetic spectra were found to match well with the above mentioned atmospheric parameters and the final abundances are given in Tables 1 and 3. A region of the observed and synthetic spectrum is shown in Fig. 3. The abundances derived using MOOG (Tables 1 and 3) are in good agreement with the abundances derived using the WIDTH (Table 1).


  \begin{figure}
\par\includegraphics[width=12.9cm,clip]{syn1a.ps}\end{figure} Figure 3: Synthetic spectrum calculated with the atmospheric parameters ( $T_{\rm eff} = 8500$ K, log g = 2.5, $V_{\rm t} = 2.5$ km s-1) and abundances (Tables 1 and 3) is overplotted on the observed spectrum in the 4380 $\AA$-4400 $\AA$ region.

3.3 Balmer lines

We tried to estimate the $T_{\rm eff}$ and log g from the analysis of Balmer lines in the spectrum of ZNG 4 using the Kurucz spectral atlas for Balmer lines (Kurucz CDROM 13, 1993).

We could not get a satisfactory fit between the observed and theoretical Balmer line profiles with the atmospheric parameters $T_{\rm eff} = 8500$ K, log g= 2.5, $V_{\rm t} = 2.5$ km  $\rm s^{-1}$ and $\rm [Fe/H]= -1.5$. We also tried models that take into account the alpha element enhancements and no convective overshooting (ANOVER models: http://kurucz.harvard.edu/grids/gridm15ANOVER/bm15ak2nover.dat). They did not make any difference to the abovementioned atmospheric parameters (Fig. 4). The best fit to $\rm H_{\beta }$ profile was obtained with the parameters $T_{\rm eff} = 8750$ K, log g= 2.0, $V_{\rm t} = 2.0$ km  $\rm s^{-1}$ and $\rm [Fe/H]= -1.5$ (Fig. 4). However, the excitation balance and ionization equilibrium for Mg and Fe lines could not be achieved with the above parameters (see the last column in Table 1) and the abundances of Mg I, Mg II and Fe I, Fe II were found to differ significantly (Table 1). Therefore, we chose the model atmosphere determined from the analysis of metal lines (i.e. $T_{\rm eff} = 8500$ K, log g= 2.5, $V_{\rm t} = 2.5$ km  $\rm s^{-1}$ and $\rm [Fe/H]= -1.5$) to represent the atmosphere of the star.

The problem of fitting Balmer line profiles of HB stars has been mentioned by Grundahl et al. (1999) (and references therein). For stars being more luminous than HB stars, mass loss and/or extended atmosphere may influence the Balmer line profiles (Vink & Cassisi 2002).


  \begin{figure}
\par\includegraphics[angle=90,width=16.3cm,clip]{bal3mod.eps}\end{figure} Figure 4: Observed $\rm H_{\beta }$ profile compared with theoretical $\rm H_{\beta }$ profiles for 2 different model atmospheric parameters. Dots and dashes represent the model with $T_{\rm eff} = 8750$ K, log g= 2.0, $\rm [M/H] = -1.5$ and $V_{\rm t} = 2.0$ km s-1 which fit the profile best. Open diamonds and asterixs represent the model $T_{\rm eff} = 8500$ K, log g= 2.5, $\rm [M/H] = -1.5$ and $V\rm _t = 2.5$ km s-1, which does not fit the observed profile. No noticable differences were observed in the theoretical $\rm H_{\beta }$ profiles by considering ANOVER models for the same atmospheric parameters and are shown by dashes for the first set of parameters and asterix in the case of second set of parameters.

4 Results

The mean abundances of ZNG 4 relative to the Sun (Anders & Grevesse 1989) are given in Table 1, together with the number of lines used in the analysis and the standard deviation of abundances estimated from individual species.


 

 
Table 2: Comparison of the abundances of ZNG 4 with the abundances of M 13 BHB and RGB stars.
Element ZNG 4 M 13/ J11 (BHB)* M 13/WF4-3485(BHB)* M 13/ L262 (RGB)* Mean
  $\rm [Fe/H]= -1.49$ $\rm [Fe/H]= -1.82$ $\rm [Fe/H]= + 0.02$ $\rm [Fe/H]= -1.61$ RGB abundances*
  $T_{\rm eff} = 8500$ K $T_{\rm eff}= 7681$ K $T_{\rm eff}= 12~750 $ K $T_{\rm eff}= 4160$ K in M 13
  log g= 2.5 log g= 3.1 log g= 4.1 log g= 0.50  
  [X/H] [X/H] [X/H] [X/H] [X/H]
He -0.55 <-0.26 -1.49 $\pm$ 0.17 ... ...
Na -1.28 ... ... -1.27 $\pm$ 0.11 -1.37 $\pm$ 0.04
Mg -1.51 -1.50 $\pm$ 0.16 -1.62 $\pm$ 0.14 -1.51 $\pm$ 0.14 -1.46 $\pm$ 0.03
Si -1.10 <-1.23 -1.43 $\pm$ 0.07 -1.16 $\pm$ 0.14 -1.30 $\pm$ 0.02
Ca -0.64 -1.72 $\pm$ 0.11 -1.66 $\pm$ 0.15 -1.39 $\pm$ 0.14 -1.34 $\pm$ 0.01
Sc -0.99 -1.63 $\pm$ 0.10 <+1.10 ... -1.67 $\pm$ 0.01
Ti -0.75 -1.32 $\pm$ 0.06 -0.53 $\pm$ 0.16 -1.30 $\pm$ 0.20 -1.32 $\pm$ 0.02
Cr -1.41 -1.71 $\pm$ 0.12 <-0.12 ... ...
Fe -1.49 -1.82 $\pm$ 0.10 +0.02 $\pm$ 0.20 -1.61 $\pm$ 0.10 -1.60 $\pm$ 0.01
Sr -2.19 -2.03 $\pm$ 0.10 <+1.75 ... ...
Y -1.20 <-0.97 <+2.92 ... -1.61 $\pm$ 0.04
Ba -1.21 -1.68 $\pm$ 0.10 <+3.26 ... -1.53 $\pm$ 0.05
* Abundances of M 13 BHB stars are from Behr (2000c) and abundances of M 13 RGB star are from Cavallo & Nagar (2000). In the last column, the mean abundances of elements from Na to Fe in M 13 RGB stars are from Kraft et al. (1997) and that of Y and Ba are from Armosky et al. (1994).



  \begin{figure}
\par\includegraphics[angle=90,width=14.6cm,clip]{ebar2.eps}\end{figure} Figure 5: The abundances of different elements in ZNG 4 (represented by asterix) compared with M 13/ J11 (BHB star; triangles), M 13/WF4-3485 (hot BHB star; diamonds) and that of M 13/ L262 (RGB star; squares) with their error bars (Table 2). In the cases where only upper limit of the abundances are given (3rd and 4th column of Table 2), those elements are not shown in the above figure. Average abundances of Y and Ba in M 13 RGB stars are from Armosky et al. (1994).

Analysis of Mg lines gives $\rm [Mg/H] = -1.5 $ which is the same as the M 13 cluster metallicity. (The equivalent widths of the Mg II lines at 4481 $\AA$ (Table 3) were obtained by multiple gaussian fit to the lines in the observed spectrum). Silicon is overabundant compared to iron ( $\rm [Si/Fe]=+0.4$). Calcium and titanium are found to be overabundant ( $\rm [Ca/Fe]=+0.8$ and $\rm [Ti/Fe]=+0.75$). There is a 0.5 dex difference in the abundances derived from the Ca I lines at 4226.73 $\AA$ and 4454.78 $\AA$ (Table 3). However, the abundance of Ca derived from the Ca II line at 5019.97 $\AA$ is in agreement with that derived from the Ca I 4454.78 $\AA$ line. The reason for the deviation in the abundance derived from the Ca I 4226.73 $\AA$line is not clear. It may be due to the relatively low signal to noise ratio of the data around this wavelength range. There seems to be no interstellar contribution to the Ca II line. Since the star has a radial velocity of -257 km s-1, the stellar lines are well separated from the lines of interstellar origin. The abundance of Cr and Fe ( $\rm [Fe/H] = -1.48$ and $\rm [Cr/Fe]=+0.09$) are found to be close to the metallicity of the cluster. On the other hand, Sc is found to be overabundant ( $\rm [Sc/Fe]=0.51$). Na lines show an overabundance of 0.2 dex. We have detected one line of Sr II, two lines of Y II and two lines of Ba II. Sr seems to be underabundant ( $\rm [Sr/Fe]=-0.70$), while Y and Ba are overabundant ( $\rm [Y/Fe]=+0.29$ and $\rm [Ba/Fe]=+0.28$).

We have detected the He I line at 4471.47 $\AA$, which yields an abundance of $\rm\log \epsilon (He) = 10.44$ which implies an underabundance of 0.55 dex compared to the solar value. This is in agreement with the underabundane of He found in hot BHB stars (Moehler 1999; Moehler et al. 2003).

We have not detected C, N and O lines in our spectrum of ZNG 4. Assuming an equivalent width of 5 m$\AA$ as the detectable limit in our spectrum of ZNG 4, we find the upper limit of $\rm [C/Fe]$ to be +0.32 dex (based on the C I 5052.17 $\AA$ line), that of $\rm [N/Fe]$ to be +1.15 dex (based on the N I 4214.80 $\AA$ line) and that of $\rm [O/Fe]$ to be +0.01 dex (based on the O I 6156.78 $\AA$ line). Globular cluster stars show anticorrelation of sodium and oxygen abundances (Kraft et al. 1997). In ZNG 4 we find enhancement of sodium, therefore we expect an underabundance of oxygen. Also star to star abundance variations in the light elements C, N, O, Na, Mg and Al occur among the bright giants of a number of globular clusters (Ivans et al. 1999). The absence of C, N and O lines in our spectrum of ZNG 4 may be due to the underabundance of these elements. A much higher resolution and high signal to noise ratio spectrum of ZNG 4 may reveal the lines of C, N and O lines if present.

5 Discussion and conclusions

The chemical composition of ZNG 4 shows significant deviations in element abundances from the expected metallicity of M 13. Ti, Ca, Sc and Ba are found to be relatively overabundant (Fig. 5) compared to RGB stars and cool BHB stars of M 13, whereas the abundances of Mg, Cr and Fe are in agreement with the cluster metallicity.

From a study of 22 M 13 G-K giants, Kraft et al. (1993, 1997) found the abundances of Fe, Sc, V and Ni to be $\rm [Fe/H]= -1.49$, $\rm [Sc/Fe] = -0.10$, [V/Fe] = 0.00 and $\rm [Ni/Fe] = -0.04$. They found Ca and Ti to be mildly overabundant ([Ca/Fe] = +0.24 and [Ti/Fe] = +0.29). Si was overabundant by +0.34 dex. Study of M 13 giants by Armosky et al. (1994) yields the average abundance of Fe, Y and Ba:  $\rm [Fe/H]= -1.49$, $\rm [Y/Fe] = -0.12$ and $\rm [Ba/Fe] = -0.04$, whereas in ZNG 4 we find significant overabundance of Ca, Sc, Ti, Y and Ba compared to that found in M 13 giants. Also, overabundance of Na [+0.2 dex] and absence of O lines support the anticorrelation of Na and O abundances found in M 13 giants (Kraft et al. 1997).

Behr et al. (1999) have studied the BHB stars in M 13 on either side of the HB gap. They find the photospheric compositions and stellar rotation rates to vary strongly as a function of  $T_{\rm eff}$ of the stars. Among the cooler stars in their sample, at $T_{\rm eff}$ of 8500 K, the metal abundances are in rough agreement with the canonical cluster metallicity and the hotter stars with $T_{\rm eff}$ greater than 10 000 K show a deficiency of He and enhancement of Fe, Ti, Cr by a factor of 300. However, Mg remains at the canonical cluster metallicity. In ZNG 4 also, Mg abundance is in agreement with the M 13 metallicity. Abundances similar to that found in BHB stars of M 13 were also found in BHB stars of M 15 (Behr et al. 2000b) and BHB stars of NGC 6752 (Glaspy et al. 1989; Moehler et al. 1999). The abundance anomalies in these BHB stars are most likely due to diffusion - the gravitational settling of helium (Greestein et al. 1967) and radiative levitation of metal atoms (Michaud et al. 1983). Rotational velocities ($v \sin i$) appear to have a bimodal distribution in cooler BHB stars, whereas the hotter BHB stars with $T_{\rm eff}$ greater than 10 000 K are found to be slow rotators.

However, the abundances and rotational velocity of ZNG 4 are contrary to what is expected for stars on the red side of the HB gap at 11 000 K. It is a slow rotator ( $v \sin i = 7$ km  $\rm s^{-1}$). It shows underabundance of He and overabundances of Ti, Ca, Sc and Ba. In Table 2 and Fig. 5, we have compared the abundances of ZNG 4 with the abundances of M 13 BHB stars of $T_{\rm eff}$ 7681 K (J 11) and $T_{\rm eff}$ 12 750 K (WF4-3485) (Behr 2000c) and with the abundances of the RGB star L262 (Cavallo & Nagar 2000). In Table 2, the last column shows the mean RGB abundances in M 13, where elements from Na to Fe are taken from Kraft et al. (1997) and Y and Ba abundances are from Armosky et al. (1994). It is evident from the abundances listed in Table 2 and from Fig. 5 that ZNG 4 shows overabundance of metals compared to that of a M 13 RGB star and also when compared to that of a M 13 BHB star of similar temperature. These results indicate that in ZNG 4, diffusion and radiative levitation of elements may be in operation. Slowly rotating HB stars are also seen on the cooler side of HB gap, but abundance anomalies start from 11 000 K (Moehler et al. 1999; Behr et al. 2000b). This implies that ZNG 4 may have the properties of the stars on the blue side of the HB gap although it has $T_{\rm eff}$ of 8500 K. In this regard, more accurate determination of abundances of these elements in ZNG 4 and similar stars in M 13 is needed to confirm our results and conclusions.

This may be explained in two ways. One is that, for some stars in M 13, the onset of diffusion seems to start at lower $T_{\rm eff}$ ($\approx $8500 K). The other argument would be that the star has evolved from the blue side of the HB gap and is moving towards the red with higher luminosity as indicated by the post-HB evolutionary tracks of Gingold (1976) and Dorman et al. (1993).

The BHB stars hotter than 11 500 K typically show strong photospheric helium depletions due to gravitational settling (Moehler et al. 2000, 2003). The calculations of Michaud et al. (1983) indicate that helium depletion should be accompanied by photospheric enhancement of metals, since the same stable atmosphere that permits gravitational settling also permits the levitation of elements with large radiative cross sections. The depletion of helium and overabudance of some of the metals in the photosphere of ZNG 4 is in qualitative agreement with the calculations of Michaud et al. (1983).

Recently, Turcotte et al. (1998) and Richer et al. (2000) made diffusion simulations to explain the abundance patterns of chemically peculiar A and F stars. Their predicted abundance patterns are qualitatively similar to that found in ZNG 4. However, none of the recent diffusion studies treated the cases of BHB stars and post-HB stars. This phenomenon may be related to the disappearance of surface convection and hence to the formation of a stable stellar atmospheres. HB stars and post-HB stars cooler than $T_{\rm eff}= 6300$ K have deep convective envelopes (Sweigart 2002). Hotter than this temperature the envelope convection breaks into distinct shells associated with the ionization of H and He. Note that the surface convection disappears at 11 000 K (Sweigart 2002) and BHB stars hotter than this show moderate to severe abundance anomalies.

ZNG 4 has a V magnitude of 13.964 (Paltrinieri et al. 1998). Considering the distance modulus of M 13 to be 14.42 and E(B-V) towards M 13 to be 0.02 (Kraft & Ivans 2003), we estimated the absolute magnitude (Mv) of the star to be -0.522. For stars with $T_{\rm eff}$ around 8500 K, the bolometric correction (BC) is negligible (Flower 1996). Considering BC=0, we get the bolometric magnitude ( $M_{\rm bol}$) to be -0.522, which corresponds to a luminosity of 127 $L_{\odot}$[ $\log {\frac {L} {L_{\odot}}} = 2.18$]. Using the equation connecting the mass, effective temperature and bolometric magnitude, we find the surface gravity, log g = 2.6 (assuming the mass of ZNG 4 to be 0.5 $M_{\odot}$), which agrees well with the value estimated from the analysis of the spectrum of ZNG 4.

The post-AGB star Barnard 29 [ $\log {\frac {L} {L_{\odot}}} = 3.3$] which is a member of M 13 is more luminous than ZNG 4. The abundance pattern of ZNG 4 is very different from that of the post-AGB star Barnard 29 (Conlon et al. 1994; Moehler et al. 1998). The M 13 BHB stars with $T_{\rm eff}$ around 8500 K have a luminosity of about 40 $L_{\odot}$, whereas ZNG 4 is more luminous by about a factor of 3, which indicates that ZNG 4 can be classified as a supra horizontal branch star (post-HB). Stars that lie 1.5 magnitude above the HB stars are classified as supra horizontal branch (SHB) stars in the photometric studies of M 13 (Zinn 1974) and NGC 6522 (Shara et al. 1998). No detailed abundance analysis of SHB stars in globular clusters is available to compare with the abundances of ZNG 4.

Since ZNG 4 is a post-HB star and it has evolved from a hot BHB star stage and may had severe abundance anomalies similar to those found in the hot BHB stars of M 13 (Table 2). The present $T_{\rm eff} = 8500$ K of ZNG 4 indicates that thin layers of subsurface convection if present may have diluted the severe abundance anomalies due to diffusion and radiative levitation that took place during its hot BHB stage of evolution. It is important to derive the chemical composition of a significant sample of post-HB stars hotter than 11 000 K and much cooler than 11 000 K to further understand the role of diffusion, radiative levitation, rotation and convection during the post-HB stage of evolution.

Acknowledgements
We would like to thank Dr. B.Dorman and Dr. B. Behr for helpful information on M 13 BHB stars, Dr. F. R. Ferraro for kindly providing the table of B and V magnitudes of M 13 cluster stars and the referee Dr. S. Moehler for helpful comments.

References

  
6 Online Material


 

 
Table 3: Data for spectral lines measured in the spectrum of ZNG 4 in M 13.

$\lambda_{\rm lab}$ (in $\AA$)

LEP (eV) log gf EW (m$\AA$) $\rm\log \epsilon $
He I        
4471.47 20.96 -0.278 11.3 10.44
Na I        
5889.95 0.00 0.117 63.9 5.05
5895.92 0.00 -0.184 40.6 5.04
Mg I        
5167.32 2.71 -1.030 31.9 6.19
5172.68 2.71 -0.402 70.2 6.09
5183.60 2.72 -0.180 85.8 6.07
Mg II        
4481.13 8.86 0.740 104.1 6.12
4481.32 8.86 0.590 80.0 5.92
Si II        
5041.02 10.07 0.291 27.5 6.59
5055.98 10.07 0.593 25.5 6.24
6347.11 8.12 0.297 84.2 6.49
6371.37 8.12 -0.003 64.1 6.48
Ca I        
4226.73 0.00 0.265 76.7 5.21
4454.78 1.90 0.335 27.7 5.71
Ca II        
5019.97 7.51 -0.501 18.6 5.77
Sc II        
4246.82 0.32 0.242 54.5 1.58
4314.08 0.62 -0.096 47.8 2.03
4320.73 0.60 -0.252 49.7 2.21
4325.00 0.59 -0.442 35.9 2.18
4374.46 0.62 -0.418 39.8 2.23
4400.39 0.60 -0.536 32.3 2.21
4415.56 0.59 -0.668 31.5 2.32
Ti II        
4161.53 1.08 -2.160 20.8 4.27
4163.65 2.59 -0.210 76.3 4.22
4171.91 2.60 -0.270 75.0 4.27
4287.87 1.08 -1.820 38.8 4.26
4290.22 1.17 -0.930 91.1 4.16
4294.10 1.08 -0.880 95.2 4.12
4300.05 1.18 -0.490 129.9 4.43
4301.91 1.16 -1.200 78.7 4.25
4307.86 1.17 -1.100 62.6 3.93
4312.86 1.18 -1.090 77.5 4.13
4314.98 1.16 -1.120 69.8 4.04
4320.96 1.17 -1.900 43.4 4.47
4330.24 2.05 -1.800 21.6 4.57
4330.69 1.18 -2.060 24.3 4.30
4344.29 1.08 -1.930 19.8 3.99
4350.83 2.06 -1.810 12.6 4.32
4367.66 2.59 -0.870 34.9 4.28
4386.84 2.60 -0.940 27.2 4.21
4391.03 1.23 -2.240 19.2 4.38
4394.05 1.22 -1.770 37.7 4.28
4395.03 1.08 -0.510 142.4 4.62
4395.85 1.24 -1.970 31.7 4.39
4399.77 1.24 -1.220 78.3 4.31
4407.68 1.22 -2.430 10.4 4.27
4411.07 3.10 -0.670 23.0 4.18
4417.72 1.17 -1.230 76.0 4.23
4418.33 1.24 -1.990 25.0 4.27
Ti II        
4421.94 2.06 -1.580 14.6 4.16
4443.79 1.08 -0.700 118.3 4.33
4450.48 1.08 -1.510 56.7 4.20
4464.45 1.16 -1.810 39.8 4.31
4488.33 3.12 -0.510 40.0 4.36
4529.47 1.57 -1.650 27.1 4.21
4533.97 1.24 -0.540 126.3 4.42
4549.62 1.58 -0.220 102.1 3.89
4563.76 1.22 -0.790 108.1 4.32
4571.97 1.57 -0.230 69.9 3.42
4589.96 1.24 -1.620 38.7 4.14
4763.88 1.22 -2.360 18.9 4.47
4779.98 2.05 -1.260 32.9 4.24
4798.52 1.08 -2.670 12.9 4.49
4805.09 2.06 -0.960 52.1 4.24
4874.01 3.10 -0.900 18.0 4.27
4911.19 3.12 -0.650 28.4 4.28
5129.15 1.89 -1.300 33.4 4.17
5154.07 1.57 -1.780 26.9 4.29
5185.91 1.89 -1.370 26.2 4.10
5188.68 1.58 -1.050 68.5 4.20
5226.54 1.57 -1.230 52.1 4.16
5336.77 1.58 -1.630 31.9 4.25
5381.02 1.57 -1.970 21.9 4.38
Cr II        
4554.99 4.07 -1.282 14.8 4.40
4558.65 4.07 -0.449 44.5 4.18
4588.20 4.07 -0.627 34.6 4.20
4616.63 4.07 -1.361 15.0 4.48
4618.80 4.07 -0.840 26.1 4.25
4634.07 4.07 -0.990 19.1 4.23
4824.13 3.87 -0.970 20.6 4.11
5237.33 4.07 -1.160 13.0 4.21
Fe I        
4143.87 1.56 -0.511 23.2 6.03
4199.10 3.05 0.155 20.4 6.30
4202.03 1.49 -0.708 20.8 6.11
4260.47 2.40 0.109 22.3 5.95
4271.76 1.49 -0.164 39.6 5.93
4325.76 1.61 0.006 48.0 5.96
4383.55 1.49 0.200 59.2 5.84
4415.12 1.61 -0.615 20.5 6.08
4891.49 2.85 -0.112 15.0 6.24
4920.50 2.83 0.068 13.6 6.00
4957.60 2.81 0.233 19.4 6.00
5269.54 0.86 -1.321 8.7 5.82
5328.04 0.92 -1.466 14.3 6.24
Fe II        
4173.46 2.58 -2.740 62.2 6.42
4178.86 2.58 -2.500 43.0 5.90
4233.17 2.58 -1.900 90.5 5.99
4296.57 2.70 -3.010 16.5 5.95
4351.77 2.70 -2.020 54.1 5.66
4385.39 2.78 -2.680 31.0 6.01
4416.83 2.78 -2.410 41.3 5.91
4489.18 2.83 -2.970 24.0 6.18
4491.40 2.86 -2.700 28.9 6.03
Fe II        
4508.29 2.86 -2.250 43.9 5.84
4515.34 2.84 -2.450 34.4 5.87
4520.22 2.81 -2.600 33.0 5.98
4522.63 2.84 -2.030 43.0 5.60
4549.47 2.83 -2.020 80.0 6.10
4555.89 2.83 -2.160 46.2 5.76
4576.34 2.84 -2.920 18.9 6.01
4582.84 2.84 -3.090 16.1 6.10
4583.84 2.81 -1.860 79.8 5.92
4629.34 2.81 -2.330 45.9 5.91
4923.93 2.89 -1.320 121.3 6.14
5018.44 2.89 -1.220 127.4 6.15
5169.03 2.89 -1.303 134.4 6.37
5197.58 3.23 -2.100 45.9 5.96
5234.62 3.22 -2.230 47.6 6.11
5276.00 3.20 -1.940 57.3 5.95
5316.61 3.15 -1.850 67.0 5.97
5362.87 3.20 -2.739 29.6 6.31
6456.38 3.90 -2.100 45.8 6.46
Sr II        
4215.52 0.00 -0.145 19.8 0.71
Y II        
4177.53 0.41 -0.160 8.98 1.09
4374.94 0.41 0.160 11.10 0.86
Ba II        
4554.03 0.00 0.170 17.03 0.95
4934.08 0.00 -0.150 8.042 0.88




Copyright ESO 2004