A Panchromatic Study of the Globular Cluster NGC 1904. I: The Blue
  Straggler Population
A Panchromatic Study of the Globular Cluster NGC 1904. I: The
Blue Straggler Population 1
B. Lanzoni1,2, N. Sanna3, F.R. Ferraro1, E. Valenti4, G. Beccari2,5,6, R.P. Schiavon7, R.T.
Rood7, M. Mapelli8, S. Sigurdsson9
1 Dipartimento di Astronomia, Università degli Studi di Bologna, via Ranzani 1, I–40127
Bologna, Italy
2 INAF–Osservatorio Astronomico di Bologna, via Ranzani 1, I–40127 Bologna, Italy
3 Dipartimento di Fisica, Università degli Studi di Roma Tor Vergata, via della Ricerca
Scientifica, 1, I–00133 Roma, Italy
4 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
5 Dipartimento di Scienze della Comunicazione, Università degli Studi di Teramo, Italy
6 INAF–Osservatorio Astronomico di Collurania, Via Mentore Maggini, I–64100 Teramo,
Italy
7 Astronomy Department, University of Virginia, P.O. Box 400325, Charlottesville, VA,
22904
8 University of Zürich, Institute for Theoretical Physics, Winterthurerstrasse 190, CH-8057
Zurich
9 Department of Astronomy and Astrophysics, The Pennsylvania State University, 525
Davey Lab, University Park, PA 16802
30 March, 07
ABSTRACT
By combining high-resolution (HST-WFPC2) and wide-field ground based
(2.2m ESO-WFI) and space (GALEX) observations, we have collected a multi-
wavelength photometric data base (ranging from the far UV to the near infrared)
of the galactic globular cluster NGC1904 (M79). The sample covers the entire
cluster extension, from the very central regions up to the tidal radius. In the
present paper such a data set is used to study the BSS population and its radial
distribution. A total number of 39 bright (m218 ≤ 19.5) BSS has been detected,
http://arxiv.org/abs/0704.1393v1
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and they have been found to be highly segregated in the cluster core. No signifi-
cant upturn in the BSS frequency has been observed in the outskirts of NGC 1904,
in contrast to other clusters (M 3, 47 Tuc, NGC 6752, M 5) studied with the
same technique. Such evidences, coupled with the large radius of avoidance es-
timated for NGC 1904 (ravoid ∼ 30 core radii), indicate that the vast majority of
the cluster heavy stars (binaries) has already sunk to the core. Accordingly, ex-
tensive dynamical simulations suggest that BSS formed by mass transfer activity
in primordial binaries evolving in isolation in the cluster outskirts represent only
a negligible (0–10%) fraction of the overall population.
Subject headings: Globular clusters: individual (NGC1904); stars: evolution –
binaries: close - blue stragglers
1. INTRODUCTION
Blue straggler stars (BSS) appear brighter and bluer than the Turn-Off (TO) point along
an extension of the Main Sequence in color-magnitude diagrams (CMDs) of stellar popula-
tions. Hence, they mimic a young stellar population, with masses larger than the normal
cluster stars (this is also confirmed by direct mass measurements; e.g. Shara, Saffer & Livio
1997). BSS are thought to be objects that have increased their initial mass during their
evolution, and two main scenarios have been proposed for their formation (e.g., Bailyn
1995): the collisional scenario suggests that BSS are the end-products of stellar mergers
induced by collisions (COL-BSS), while in the mass-transfer scenario BSS form by the
mass-transfer activity between two companions in a binary system (MT-BSS), possibly up
to the complete coalescence of the two stars (Mateo et al. 1990; Pritchet & Glaspey 1991;
Bailyn & Pinsonneault 1995; Carney Latham; Tian et al. 2006; Leigh, Sills & Knigge 2007).
Hence, understanding the origin of BSS in stellar clusters provides valuable insight both on
the binary evolution processes and on the effects of dynamical interactions on the (otherwise
normal) stellar evolution. The MT formation scenario has by recently received further sup-
port by high-resolution spectroscopic observations, which detected anomalous Carbon and
Oxygen abundances on the surface of a number of BSS in 47 Tuc (Ferraro et al. 2006a).
However the role and relative importance of the two mechanisms are still largely unknown.
1Based on observations with the NASA/ESA HST, obtained at the Space Telescope Science Institute,
which is operated by AURA, Inc., under NASA contract NAS5-26555. Also based on GALEX observations
(program GI-056) and WFI observations collected at the European Southern Observatory, La Silla, Chile,
within the observing programs 62.L-0354 and 64.L-0439.
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To clarify the BSS formation and evolution processes we studying the BSS radial distri-
bution over the entire cluster extension in a number of galactic globular clusters (GCs). We
completed such studies in 5 GCs: M 3 (Ferraro et al. 1997), 47 Tuc (Ferraro et al. 2004),
NGC 6752 (Sabbi et al. 2004), ω Cen (Ferraro et al. 2006b), and M 5 (Lanzoni et al. 2007,
see also Warren, Sandquist & Bolte 2006). Apart from ωCen where mass segregation pro-
cesses have not yet played a major role in altering the initial BSS distribution, the BSS
are always highly concentrated in the cluster central regions. Moreover, in M 3, 47 Tuc,
NGC 6752, and M 5 the BSS fraction decreases at intermediate radii and rises again in the
outskirsts of the clusters, yielding a bimodal distribution. Preliminary evidences of such a
bimodality have been found also in M 55 by Zaggia, Piotto & Capaccioli (1997). Recent
dynamical simulations (Mapelli et al. 2004, 2006; Lanzoni et al. 2007) have been used to
interpret the observed trends and have shown that a significant fraction ( >∼ 50%) of COL-
BSS is required to account for the observed BSS central peaks. In addition, a fraction of
20-40% MT-BSS is needed to reproduce the outer increase observed in these clusters. The
case of ω Cen is reproduced by assuming that the BSS population in this cluster is com-
posed entirely of MT-BSS. These results demonstrate that detailed studies of the BSS radial
distribution within GCs are very powerful tools for better understanding the BSS formation
channels and for probing the complex interplay between dynamics and stellar evolution in
dense stellar systems.
In this paper we present multi-wavelength observations of NGC 1904. These observa-
tions are part of a coordinated project aimed at properly characterize the UV excess of old
stellar aggregates as globular clusters, in terms of their hot stellar populations, like Hori-
zontal Branch (HB) and Extreme HB stars, post-Asymptotic Giant Branch stars, BSS, etc.
From integrated light measurements obtained with UIT (see Dorman, O’Connell & Rood
1995), NGC 1904 was known to be relatively bright in the UV, and it was selected as a prime
target in both our high-resolution (using HST) and wide-field (using GALEX) UV surveys.
We have obtained a large set of data: (i) high-resolution ultraviolet (UV) and optical images
of the cluster center have been secured with the WFPC2 on board HST; (ii) complementary
wide-field observations covering the entire cluster extension have been obtained in the UV
and optical bands by using the far- and near-UV detectors on board the Galaxy Evolution
Explorer (GALEX) satellite and with ESO-WFI mounted at the 2.2m ESO telescope, re-
spectively. The combination of these datasets allowed a study of the structural properties
of NGC 1904 (thus leading to an accurate redetermination of the center of gravity and the
surface density profile), and of the radial distribution of the evolved stellar populations (in
particular the BSS and horizontal branch star distributions have been derived over the en-
tire cluster extension). While a companion paper (Schiavon et al. 2007, in preparation) will
focus on the morphology and the structure of the HB, the present paper is devoted to the
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BSS population.
2. OBSERVATIONS AND DATA ANALYSIS
2.1. The data sets
The present study is based on a combination of different photometric data sets:
1. The high-resolution set – It consists of a series of UV, near UV and optical images
of the cluster center obtained with HST-WFPC2 with two different pointings. In both cases
the Planetary Camera (PC, the highest resolution instrument with 0.′′046 pixel−1) has been
pointed approximately on the cluster center to efficiently resolve the stars in the highly
crowded central regions; the three Wide Field Cameras (WFC with resolution 0.′′1 pixel−1)
have been used to sample the surrounding regions. Observations in Pointing A (Prop. 6607,
P.I. Ferraro) have been performed through filters F160BW (far-UV), F336W (approximately
an U filter) and F555W (V ), for a total exposure time texp = 3300, 4400, and 300 sec, respec-
tively. Pointing B is a set of public HST-WFPC2 observations (Prop. 6095, P.I. Djorgovski)
obtained through filters F218W (mid-UV), F439W (B) and F555W (V ). Because of the dif-
ferent orientations of the four cameras, this data set is complementary to the former (with
the PC field of view in common), thus offering full coverage of the innermost regions of
the cluster (see Figure 1). The combined photometric sample is ideal for efficiently studying
both the hot stellar populations (as the BSS and the HB stars) and the cool red giant branch
(RGB) population, and to guarantee a proper combination with the wide-field data set (see
below).
The photometric reduction of both the high-resolution sets was carried out using RO-
MAFOT (Buonanno et al. 1983), a package developed to perform accurate photometry in
crowded fields and specifically optimized to handle under-sampled Point Spread Functions
(PSFs; Buonanno & Iannicola 1989), as in the case of the HST-WFC chips. The standard
procedure described in Ferraro et al. (1997, 2001) was adopted to derive the instrumen-
tal magnitudes and to calibrate them to the STMAG system by using the zero-points of
Holtzman et al. (1995). The magnitude lists were finally cross-correlated in order to obtain
a combined catalog.
2. The wide-field set - A complementary set of wide-field U, B, and I images was
secured by using the Wide Field Imager (WFI) at the 2.2m ESO-MPI telescope, during
an observing run in January 1999 (Progr. ID: 062.L-0354, PI: Ferraro). A set of WFI V
images (Progr. ID: 064.L-0255) was also retrieved from the ESO-STECF Science Archive.
Additional deep wide-field images were obtained in the UV band with the satellite GALEX
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(GI-056, P.I. Schiavon) through the FUV (1350–1750 Å) and NUV (1750–2800 Å) detectors.
With a global field of view (FoV) of 34′ × 34′, the WFI observations cover the entire cluster
extension. There is also full coverage of the cluster in the UV thanks to the large GALEX
FoV, which is approximately 1 deg in diameter and includes theWFI FoV (see Figure 2, where
the cluster is roughly centered on WFI CCD #2). However, because of the low resolution of
the instrument (4′′ and 6′′ in the FUV and NUV channels, respectively), GALEX data have
been used to sample only the external cluster regions not covered by HST.
The raw WFI images were corrected for bias and flat field, and the overscan regions were
trimmed using IRAF2 tools (mscred package). Standard crowded field photometry, including
PSF modeling, was carried out independently on each image using DAOPHOTII/ALLSTAR
(Stetson 1987). For each WFI chip a catalog listing the instrumental U, B, V, and I
magnitudes was obtained by cross-correlating the single-band catalogs. Several hundred
stars in common with Kravtsov et al. (1997), Stetson (2000), and Ferraro et al. (1992) have
been used to transform the instrumental U , B, V , and I magnitudes to the Johnson/Cousins
photometric system.
As for the WFI data, also for GALEX observations standard photometry and PSF fitting
were performed independently on each image using DAOPHOTII/ALLSTAR. A combined
FUV-NUV catalog was then obtained by cross-correlating the single-band catalogs.
2.2. Astrometry and homogenization of the catalogs
The HST, WFI, and GALEX catalogs have been placed on the absolute astrometric
system by adopting the procedure already described in Ferraro et al. (2001, 2003). The
new astrometric Guide Star Catalog (GSC-II3) was used to search for astrometric standard
stars in the WFI FoV, and a cross-correlation tool specifically developed at the Bologna
Observatory (Montegriffo et al. 2003, private communication) has been employed to obtain
an astrometric solution for each WFI chip. Several hundred GSC-II reference stars were
found in each chip, thus allowing an accurate absolute positioning of the stars. Then, we
used more than 3000 and 1500 bright WFI stars in common with the HST and GALEX
samples, respectively, as secondary astrometric standards, so as to place all the catalogs
on the same absolute astrometric system. We estimate that the global uncertainties in the
2IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Associa-
tion of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science
Foundation.
3Available at http://www-gsss.stsci.edu/Catalogs/GSC/GSC2/GSC2.htm.
http://www-gsss.stsci.edu/Catalogs/GSC/GSC2/GSC2.htm
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astrometric solution is of the order of ∼ 0.′′2, both in right ascension (α) and declination (δ).
Once placed on the same coordinate system, the catalogs have been cross-correlated and
the stars in common have been used to transform all the magnitudes in the same photometric
system. In particular, the HST STMAG magnitudes have been converted to the WFI ones
by using the stars in common between the two samples in the optical bands. Then, the
GALEX FUV and NUV instrumental magnitudes have been calibrated onto the HST m160
and m218 magnitudes, respectively using the stars in common between the GALEX and HST
samples.
At the end of the procedure a homogeneous master catalog of magnitudes and absolute
coordinates of all the stars included in the HST, WFI, and GALEX samples was finally
produced.
2.3. Center of gravity and definition of the samples
Once the absolute positions of individual stars have been obtained, the center of gravity
Cgrav of NGC 1904 has been determined by averaging the coordinates α and δ of all stars lying
in the PC FoV, following the iterative procedure described in Montegriffo et al. (1995, see
also Ferraro et al. 2003, 2004). In order to correct for spurious effects due to incompleteness
in the very inner regions of the cluster, we considered two samples with different limiting
magnitudes (V < 19 and V < 20), and we computed the barycenter of stars for each
sample. The two estimates agree within ∼ 1′′, setting Cgrav at α(J2000) = 05
h 24m 11.s09,
δ(J2000) = −24o 31′ 29.′′00. The newly determined center of gravity is located at ∼ 7′′ south-
est (∆α = 7.′′3, ∆δ = −2′′) from that previously derived by Harris (1996) on the basis of
the surface brightness distribution.
In order to reduce spurious effects in the most crowded regions of the cluster due to the
low resolution of the WFI and GALEX observations, we considered only the HST data for
the inner 85′′ from the center, this value being imposed by the geometry of the combined
WFPC2 FoVs (see Figure 1). Thus, in the following we define as HST sample the ensemble
of all the stars observed with HST at r ≤ 85′′ from Cgrav, and as External sample all the
stars detected with WFI and/or GALEX at r > 85′′, out to ∼ 1100′′ (see Figure 2). The
CMDs of the HST and External samples in the (V, B − V ) planes are shown in Figure 3.
Note that only the data suitable for the study of the BSS population will be considered
in the following, while those obtained through filters F160BW and FUV on board HST and
GALEX, respectively, will be used in a forthcoming paper specifically devoted to the analysis
the HB properties (Schiavon et al. 2007).
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2.4. Density profile
Considering all the stars brighter than V = 20 in the combined HST+External catalog
(see Figure 3), we have determined the projected density profile of NGC 1904 by direct
star counts over the entire cluster extension. Following the procedure already described in
Ferraro et al. (1999a, 2004), we have divided the entire sample in 31 concentric annuli, each
centered on Cgrav and split in an adequate number of sub-sectors (quadrants for the annuli
totally sampled by the observations, octants elsewhere). The number of stars lying within
each sub-sector was counted, and the star density was obtained by dividing these values by
the corresponding sub-sector areas. The stellar density in each annulus was then obtained
as the average of the sub-sector densities, and the standard deviation was estimated from
the variance among the sub-sectors.
The radial density profile thus derived is plotted in Figure 4, and the average of the
three outermost (r > 8.′3) surface density measures has been adopted as the background
contribution (corresponding to 0.95 arcmin−2). Figure 4 also shows the mono-mass King
model that best fits the derived density profile, with the corresponding values of the core
radius and concentration being rc ≃ 9.
′′7 (with a typical error of ∼ ±2′′) and c = 1.71,
respectively (hence, the tidal radius is rt ≃ 500
′′ ≃ 50 rc). These values are in good agreement
with those quoted by Harris (1996, rc = 9.
′′6 and c = 1.72), Trager, Djorgovski & King
(1993, rc = 9.
′′55 and c = 1.72), and McLaughlin & van der Marel (2005, rc = 10.
′′3 and c =
1.68), derived from the surface brightness profile, and they confirm that NGC 1904 has not
yet experienced core collapse. By assuming a distance modulus (m−M)0 = 15.63 (distance
d ∼ 13.37 kpc, Ferraro et al. 1999b), the derived value of rc corresponds to ∼ 0.65 pc. By
summing the luminosities of stars with V ≤ 20 observed within ∼ 4′′, we estimate that the
extinction-corrected central surface brightness of the cluster is µV,0(0) ≃ 16.20 mag/arcsec
in good agreement with Harris (1996, µV,0 = 16.23), Djorgovski (1993, µV,0 = 16.15), and
McLaughlin & van der Marel (2005, µV,0 = 16.18). Following the procedure described in
Djorgovski (1993, see also Beccari et al. 2006), we derive log ν0 ≃ 3.97, where ν0 is the
central luminosity density in units of L⊙/pc
3 (for comparison, log ν0 = 4.0 in Harris 1996;
Djorgovski 1993; McLaughlin & van der Marel 2005).
3. THE BSS POPULATION OF NGC 1904
3.1. BSS selection
At UV wavelengths BSS are among the brightest objects in a GC, and RGB stars are
particularly faint. By combining these advantages with the high-resolution capability of HST,
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the usual problems associated with photometric blends and crowding in the high density
central regions of GCs are minimized, and BSS can be most reliably recognized and separated
from the other populations in the UV CMDs. For these reasons our primary criterion for
the definition of the BSS sample is based on the position of stars in the (m218, m218 − B)
plane (see also Ferraro et al. 2004, for a detailed discussion of this issue). In order to avoid
incompleteness bias and the possible contamination from TO and sub-giant branch stars,
we have adopted a limiting magnitude m218 = 19.5, roughly corresponding to 1 magnitude
brighter than the cluster TO. The resulting BSS selection box in the UV CMD is shown
in Figure 5. Once selected in the UV CMD, all the BSS lying in the field in common with
the optical-HST sample have been used to define the selection box in the (V, B − V ) and
(V, U − V ) planes. The limiting magnitude in the V band is V ≃ 18.9, and the adopted
BSS selection boxes in these planes are shown in Figures 3 and 6 (only stars not observed
in HST-Pointing B are shown in the latter).
With these criteria we have identified 39 BSS in NGC 1904: 37 in the HST sample
(32 from HST-Pointing B, and 5 from HST-Pointing A) and 2 in the External sample (r >
85′′), the most distant lying at r ≃ 270′′ (∼ 4.′5) from the cluster center (see Figure 2).
All candidate BSS have been confirmed by visual inspection, evaluating the quality and
the precision of the PSF fitting. This procedure significantly reduces the possibility of
introducing spurious objects, such as blends, background galaxies, etc., in the sample. The
coordinates and magnitudes of all the identified BSS are listed in Table 1.
In order to study the radial distribution of BSSs, one needs to compare their number
counts as a function of radius with those of a population assumed to trace the radial density
distribution of normal cluster stars. We chose to use HB stars for that purpose, given
their high luminosities and relatively large number. Thanks to the (essentially blue) HB
morphology, such a population can be easily selected in all CMDs, and the adopted selection
boxes, designed to include the bulk of HB and the few post-HB stars, are shown in Figures
5–6. In order to be conservative, a few stars lying within the adopted HB selection boxes
in the optical bands, but not detected in the UV filters (GALEX-NUV channel and HST-
F218W filter), have been excluded from the following analysis. However slightly different
boxes or the inclusion of these stars in the sample have no effects on the results. With these
criteria we have identified 249 HB stars (197 at r ≤ 85′′ from the HST sample, and 52 at
85′′ < r ≤ rt from the External sample).
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3.2. BSS mass distribution
The position of BSS in the CMD can be used to derive a ”photometric ” estimate of their
masses through the comparison with theoretical isochrones. We did this in the (V, B − V )
plane, where 34 BSS (32 from the HST-Pointing B and 2 from the External sample) out of
the 39 identified in the cluster have been measured.
A set of isochrones of appropriate metallicity (Z = 6 × 10−4) has been extracted from
the data-base of Cariulo, Degl’Innocenti & Castellani (2003) and transformed into the ob-
servational plane by adopting a reddening E(B − V ) = 0.01 (Ferraro et al. 1999b). The 12
Gyr isochrone nicely reproduces the main cluster population, while the region of the CMD
populated by the BSS is well spanned by a set of isochrones with ages ranging from 1 to 6
Gyr (see Figure 7). Thus, the entire dataset of isochrones available in this age range (stepped
at 0.5 Gyr) has been used to derive a grid linking the BSS colors and magnitudes to their
masses. Each BSS has been projected on the closest isochrone and a value of its mass has
been derived. As shown in the lower panel of Figure 7, BSS masses range from ∼ 0.95 to
∼ 1.6M⊙, and both the mean and the median of distribution correspond to 1.2 M⊙. The
TO mass turns out to be MTO = 0.8M⊙.
3.3. The BSS radial distribution
The radial distribution of BSS identified in NGC 1904 has been studied following
the same procedure previously adopted for other clusters (see references in Ferraro 2006;
Beccari et al. 2006). In Figure 8 we compare the BSS cumulative radial distribution to that
of HB stars. The two distributions are obviously different, with the BSS being more centrally
concentrated than HB stars. A Kolmogorov-Smirnov test gives a ∼ 7×10−4 probability that
they are extracted from the same population, i.e. the two populations are different at more
than 3σ level.
For a more quantitative analysis, the surveyed area has been divided into 6 concentric
annuli, the first roughly corresponding to the core radius (r = 10′′), and the others chosen
in order to sample approximately the same fraction of the cluster luminosity out to the tidal
radius (rt ≃ 500
′′). The luminosity in each annulus has been calculated by integrating the
surface density profile shown in Figure 4. The number of BSS and HB stars (NBSS and NHB,
respectively), as well as the fraction of sampled luminosity (Lsamp) measured in each annulus
are listed in Table 2 and have been used to compute the population ratio NBSS/NHB and the
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specific frequencies (see Ferraro et al. 2003):
Rpop =
(Npop/N
(Lsamp/L
tot )
, (1)
with pop = BSS, HB.
The resulting radial trend of RHB over the surveyed area is essentially constant, with a
value close to unity (see Figure 9). This is just what expected on the basis of the stellar evolu-
tion theory, which predicts that the fraction of stars in any post-main sequence evolutionary
stage is strictly proportional to the fraction of the sampled luminosity (Renzini & Fusi Pecci
1988). In contrast the BSS show a completely different radial distribution: as shown in
Figure 9, the specific frequency RBSS is highly peaked at the cluster center decreases to a
minimum at r ≃ 12 rc and remains approximately constant outwards. The same behavior
is clearly visible also in Figure 10, where the population ratio NBSS/NHB is plotted as a
function of r/rc.
3.4. Dynamical simulations
Following the same approach as Mapelli et al. (2004, 2006) and Lanzoni et al. (2007),
we have used a Monte-Carlo simulation code (originally developed by Sigurdsson & Phinney
1995) in order to reproduce the observed radial distribution and to derive some clues about
the BSS formation mechanisms. Such a code follows the dynamical evolution of N BSS
within a background cluster, taking into account the effects of both dynamical friction and
distant encounters. Since stellar collisions are most probable in the central high-density
regions of the clusters, in the simulations we define COL-BSS those objects with initial
positions ri
∼ rc. Since primordial binaries most likely evolve in isolation if they orbit in
the cluster outskirts, we identify as MT-BSS those BSS having ri ≫ rc. Within these
defintions, in any given run we assume that a certain fraction of the N simulated BSS is
made of COL-BSS and the remaining fraction of MT-BSS. The initial positions ri of the
two types of BSS are randomly generated within the appropriate radial range (ri
∼ rc for
COL-BSS, and ri ≫ rc for the others) following a flat distribution, according to the fact
that the number of stars in a King model scales as dN = n(r) dV ∝ r−2πr2dr ∝ dr. Their
initial velocities are randomly extracted from the cluster velocity distribution illustrated
in Sigurdsson & Phinney (1995), and an additional natal kick is assigned to COL-BSS to
account for the recoil induced by the three-body encounters that trigger the merger and
produce the BSS (see, e.g., Sigurdsson, Davies & Bolte 1994; Davies, Benz & Hills 1994).
Each BSS has characteristic mass M and maximum lifetime tlast. We follow their dynamical
evolution in the (fixed) gravitational potential for a time ti (i = 1, N), where each ti is a
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randomly chosen fraction of tlast. At the end of the simulation we register the final positions
of BSS, and we compare their radial distribution with the observed one. The percentage
of COL- and MT-BSS is changed and the procedure repeated until a reasonable agreement
between the simulated and the observed distributions is reached.
For a more detailed discussion of the procedure and the ranges of values appropriate for
the input parameters we refer to Mapelli et al. (2006). Here we only list the assumptions
made in the present study:
– the background cluster has been approximated with a multi-mass King model, deter-
mined as the best fit to the observed profile4. The cluster central velocity dispersion
is set to σ = 3.9 km s−1 (Dubath, Meylan & Mayor 1997), and, assuming 0.5M⊙ as
the average mass of the cluster stars, the central stellar density is nc = 3 × 10
4 pc−3
(Pryor & Meylan 1993);
– BSS masses have been fixed toM = 1.2M⊙ (see Section 3.2) and characteristic lifetimes
tlast ranging between 1.5 and 4 Gyr have been considered;
– COL-BSS have been distributed with initial positions ri ≤ rc and have been given a
natal kick velocity of 1× σ;
– initial positions ranging between 5 rc and rt have been considered for MT-BSS in dif-
ferent runs;
– in each simulation we have followed the evolution of N = 10, 000 BSS.
The simulated radial distribution that best reproduces the observed one (with a reduced
χ2 ≃ 0.1) is shown in Figure 10 and is obtained by assuming that the totality of BSS is
made of COL-BSS. In the best-fit case the BSS characteristic lifetime is tlast ≃ 1.5 Gyr,
but a variation between 1 and 4 Gyr of this parameter still leads to a very good agreement
(χ2 ≃ 0.2–0.3) with the observations. For the sake of comparison, in Figure 10 we also show
the results of the simulations obtained by assuming a percentage of MT-BSS ranging from
10% to 40% (see lower and upper boundaries of the gray region, respectively)5. As can be
4By adopting the same mass groups as those of Mapelli et al. (2006), the resulting value of the King
dimensionless central potential is W0 = 10
5Note that a population of 40% MT-BSS was needed in order to reproduce the bimodal distribution
observed in M 3, 47 Tuc and NGC 6752 (Mapelli et al. 2006), and 10% was found to be the appropriate
percentage of MT-BSS in the case of M 5 (Lanzoni et al. 2007).
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seen, while a population of 10% MT-BSS is still marginally consistent with the observations,
larger percentages systematically overestimate the BSS population at r >∼ 5 rc. Increasing
the BSS mass up to 1.5M⊙ does not change this conclusion.
By assuming 12 Gyr for the age of NGC 1904, we have used the simulations and the
dynamical friction timescale (from, e.g., Mapelli et al. 2006) for 1.2M⊙ stars to estimate
the radius of avoidance ravoid of the cluster, i.e., the radius within which all these stars are
expected to have already sunk to the cluster core because of mass segregation processes. We
find that ravoid ∼ 30 rc (i.e., ∼ 300
′′), which corresponds to a significant fraction of the entire
cluster extension. This evidence is consistent with the fact that the simulated MT-BSS
appear to be a negligible fraction of the overall BSS population.
4. DISCUSSION
We have studied the brightest portion (m218 ≤ 19.5) of the BSS population in NGC 1904.
We have found a total of 39 objects, with a high degree of segregation in the cluster center.
Approximately 38% of the entire BSS population is found within the cluster core, while only
∼ 13% of HB stars are counted in the same region. This indicates a significant overabundance
of BSS in the center, as also confirmed by the fact that the BSS specific frequency RBSS within
rc is roughly 3 times larger than expected for a normal (non-segregated) population on the
basis of the sampled light (see Figure 9). The peak value is in good agreement with what is
found in the case of M 3, 47 Tuc, NGC 6752 and M 5 (see Ferraro et al. 2004; Sabbi et al.
2004; Lanzoni et al. 2007). Unlike these clusters, no significant upturn of the distribution
at large radii has been detected in NGC 1904.
We emphasize that the absence of an external upturn in the BSS radial distribution is
not an effect of low statistics. In the case of NGC 6752, where a similar amount of BSS (34)
has been detected, the BSS radial distribution is clearly bimodal (Sabbi et al. 2004). This
can be seen also in Figure 11, where the two distributions are directly compared. They nicely
agree within r ∼ 12rc, but the fraction of BSS in NGC 6752 rises again at larger distances
from the center, despite the smaller number of BSS observed in this cluster compared to
NGC 1904.
Extensive dynamical simulations have been used to derive some hints about the BSS
formation mechanisms. Even if admittedly crude, this approach has been successfully used to
demonstrate that the external rising branch of the BSS radial distribution observed in M 3,
47 Tuc, NGC 6752 and M 5 cannot be due to COL-BSS originated in the core and then kicked
out in the outer regions: hence, a significant fraction (20-40%) of the overall population is
– 13 –
required to be made of MT-BSS in these clusters (Mapelli et al. 2006; Lanzoni et al. 2007).
By using the same simulations to interpret the (flat) BSS radial distribution of NGC 1904,
we found that only a negligible percentage (0–10%) of MT-BSS is needed. However, we
emphasize that if a rising peripheral BSS frequency is absent (as in the case of NGC 1904)
our simple approach cannot distinguish between BSS created by MT (and then segregated
into the cluster core by the dynamical friction) and COL-BSS created by collisions inside
the core.
On the other hand, the negligible fraction of peripheral MT-BSS found in NGC 1904 is
in agreement with the quite large value of the radius of avoidance estimated for this cluster
(ravoid ≃ 30 rc), which indicates that all the heavy stars (binaries) within this radial distance
have had enough time to sink to the core and are therefore not expected in the cluster
outskirts. Such a radial distance corresponds to 0.6 rt, i.e., it represents a significant fraction
of the cluster extension (only 1% of the cluster light is contained between ravoid and rt),
and hence only a small fraction of the massive objects are expected to be unaffected by the
dynamical friction). In all the other studied cases, ravoid is significantly smaller: ravoid
∼ 0.2 rt
(Mapelli et al. 2006; Lanzoni et al. 2007). In turn, this suggests that at least a fraction of
the BSS population that we now observe in the cluster center are primordial binaries which
have sunk to the core because of the dynamical friction process, and mixed with those that
formed through stellar collisions.
Only systematic surveys of physical and chemical properties for a large number of BSS
in different environments (see examples in De Marco et al. 2005; Ferraro et al. 2006a) can
definitively identify the formation processes of these stars.
This research was supported by Agenzia Spaziale Italiana under contract ASI-INAF
I/023/05/0, by the Istituto Nazionale di Astrofisica under contract PRIN/INAF 2006, and
by the Ministero dell’Istruzione, dell’Università e della Ricerca. RTR is partially funded by
NASA through grant number HST-GO-10524 from the Space Telescope Science Institute.
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This preprint was prepared with the AAS LATEX macros v5.2.
– 17 –
Fig. 1.—Map of the combined HST sample. The light solid and dotted lines delimit the FoVs
of Pointing B and A, respectively. Star positions are plotted with respect to the center of
gravity Cgrav derived in Section 2.3: α(J2000) = 05
h 24m 11..s09, δ(J2000) = −24o 31′ 29.′′00.
The positions of all BSS identified in this sample are marked with heavy dots and the
concentric annuli used to study their radial distribution (cfr. Table 1) are also shown. The
inner and outer annuli correspond to r = rc = 10
′′ and r = 85′′, respectively.
– 18 –
Fig. 2.— Map of the External sample. The light solid and dotted lines delimit the WFI and
the GALEX FoVs, respectively. The two BSS detected in the External sample are marked
as heavy dots, and the concentric annuli used to study their radial distribution are shown
as heavy circles. The inner annulus is at 85′′ and corresponds to the most external one in
Figure 1. The heavy dashed circle marks the tidal radius of the cluster (rt ≃ 500
– 19 –
Fig. 3.— (V, B − V ) CMDs of the HST (Pointing B) and External samples. The hatched
regions (V ≥ 20) indicate the stars not used to derive the cluster surface density profile. The
adopted BSS and HB selection boxes are shown, and all the identified BSS are marked with
the empty circles.
– 20 –
Fig. 4.— Observed surface density profile (dots and error bars) and best-fit King model
(solid line). The radial profile is in units of number of stars per square arcsec. The dotted
line indicates the adopted level of the background, and the model characteristic parameters
(core radius rc, concentration c, dimensionless central potential W0), as well as the χ
2 value
of the fit are marked in the figure. The location of the cluster tidal radius is marked by the
arrow. The lower panel shows the residuals between the observations and the fitted profile
at each radial coordinate.
– 21 –
Fig. 5.— CMD of the ultraviolet (Pointing B) HST sample. The adopted magnitude limit
and selection box used for the definition of the BSS population (empty circles) are shown.
The two solid triangles correspond to BSS-38 and 39 found in the External Sample, with
UV magnitudes obtained through the GALEX NUV detector. The selection boxes adopted
for HB and post-HB stars are also shown.
– 22 –
Fig. 6.— (V, U − V ) CMD of the HST (Pointing A) sample (only stars not observed in
Pointing B are plotted). The adopted BSS and HB selection boxes are shown, and all the
identified BSS and HB stars are marked with the empty circles and squares, respectively.
– 23 –
Fig. 7.— Upper panel: zoomed (V, B − V ) CMD of the BSS region; the 34 BSS measured
in this plane are shown. The set of isochrones ranging from 1 to 6 Gyr (stepped by 0.5 Gyr)
from Cariulo, Degl’Innocenti & Castellani (2003) data base used to derive BSS masses is
also shown. Lower panel: derived mass distribution for the BSS shown in the upper panel.
– 24 –
Fig. 8.— Cumulative radial distribution of BSS (solid line) and HB (dashed line) stars as a
function of the projected distance from the cluster center for the combined HST+External
sample. The location of the cluster tidal radius is marked by the arrow.
– 25 –
Fig. 9.— Radial distribution of the BSS (dots) and HB (gray regions) specific frequencies,
as defined in equation (1), and as a function of the radial distance in units of the core radius.
The vertical size of the gray regions correspond to the error bars.
– 26 –
Fig. 10.— Radial distribution of the population ratio NBSS/NHB as a function of r/rc (dots
with error bars), compared with the simulated distribution (solid line and triangles) obtained
by assuming 100% of COL-BSS. The results of the simulations obtained by assuming a
percentage of MT-BSS ranging from 10% to 40% (lower and upper boundaries of the gray
region, respectively) are also shown.
– 27 –
Fig. 11.— Radial distribution of the population ratio NBSS/NHB for NGC 1904 (filled circles)
and NGC 6752 (open circles) plotted as a function of the radial distance in core radius units.
– 28 –
Table 1. The BSS population in NGC1904
Name RA DEC m218 U B V I
[degree] [degree]
BSS-1 81.048797100 -24.526391100 19.11 18.64 18.66 18.45 -
BSS-2 81.047782800 -24.526527400 18.65 18.12 18.21 17.94 -
BSS-3 81.047540400 -24.526005300 18.85 18.34 18.38 18.22 -
BSS-4 81.048954000 -24.525188200 17.94 17.75 17.87 17.78 -
BSS-5 81.047199200 -24.525797600 17.58 17.47 17.40 17.35 -
BSS-6 81.045528300 -24.525876800 18.64 18.24 18.28 18.12 -
BSS-7 81.044296100 -24.526362200 19.13 18.77 18.76 18.55 -
BSS-8 81.048506700 -24.524266800 19.18 18.55 18.64 18.39 -
BSS-9 81.041556100 -24.526972400 19.35 18.65 18.86 18.49 -
BSS-10 81.045827300 -24.525062700 18.06 17.35 17.17 16.96 -
BSS-11 81.045467700 -24.525147900 17.84 17.44 17.56 17.41 -
BSS-12 81.047088300 -24.524375900 18.80 18.20 18.01 17.80 -
BSS-13 81.046548400 -24.524483700 19.43 18.77 18.67 18.38 -
BSS-14 81.045121300 -24.524748300 19.28 18.33 18.65 18.21 -
BSS-15 81.045883300 -24.524278600 18.97 18.42 18.30 18.13 -
BSS-16 81.046164500 -24.522567300 18.41 17.72 17.63 17.42 -
BSS-17 81.044313700 -24.523304200 18.66 18.46 18.44 18.27 -
BSS-18 81.047157500 -24.521982700 18.49 18.45 18.41 18.32 -
BSS-19 81.043418100 -24.523247200 17.88 18.16 17.68 17.55 -
BSS-20 81.046665900 -24.520192000 19.49 18.71 18.92 18.60 -
BSS-21 81.044991400 -24.520127500 18.93 18.45 18.44 18.21 -
BSS-22 81.046157800 -24.519245100 19.49 18.92 19.06 18.74 -
BSS-23 81.049326100 -24.521621900 18.08 - 18.01 17.99 -
BSS-24 81.049155900 -24.520629500 18.41 - 17.98 17.87 -
BSS-25 81.047244500 -24.517052600 19.41 18.97 19.11 18.82 -
BSS-26 81.051592200 -24.523146600 18.67 - 18.33 18.21 -
BSS-27 81.050476100 -24.517107000 19.01 18.65 18.54 18.39 -
BSS-28 81.060767000 -24.520983900 18.92 - 18.59 18.45 -
BSS-29 81.068117100 -24.517558600 19.39 - 18.91 18.60 -
BSS-30 81.043233100 -24.533852000 17.34 - 16.75 16.65 -
BSS-31 81.044917900 -24.540315000 18.34 - 17.48 17.22 -
BSS-32 81.038520800 -24.540891600 17.77 17.46 17.30 17.20 -
BSS-33 81.045196533 -24.515874863 - 17.91 - 17.84 -
BSS-34 81.032196045 -24.512256622 - 18.75 - 18.41 -
BSS-35 81.037574768 -24.525493622 - 18.87 - 18.58 -
BSS-36 81.041069031 -24.518457413 - 18.80 - 18.64 -
BSS-37 81.045227051 -24.517648697 - 18.86 - 18.68 -
BSS-38 81.056510925 -24.449676514 19.04† 18.78 18.56 18.35 18.08
– 29 –
Table 1—Continued
BSS-39 81.058883667 -24.555763245 19.39† 19.14 19.05 18.73 18.34
Note. — † Note that, while the header of the column referes to HST-F218W
magnitudes, those of BSS-38 and -39 have been obtained with the NUV channel
of GALEX and transformed to the m218 scale as described in Section 2.2.
ri re NBSS NHB L
samp/L
0 10 15 34 0.14
10 20 10 45 0.18
20 40 7 62 0.22
40 85 5 56 0.23
85 150 1 34 0.13
150 500 1 18 0.10
Table 2: Number of BSS and HB stars, and fraction of luminosity sampled in the 6 concentric
annuli used to study the BSS radial distribution of NGC 1904 (ri and re correspond to the
internal and external radius of each considered annulus, in arcsec).
	INTRODUCTION
	OBSERVATIONS AND DATA ANALYSIS
	The data sets
	Astrometry and homogenization of the catalogs 
	Center of gravity and definition of the samples
	Density profile
	THE BSS POPULATION OF NGC 1904 
	BSS selection
	BSS mass distribution
	The BSS radial distribution
	Dynamical simulations
	DISCUSSION
