Old Main-Sequence Turnoff Photometry in the Small Magellanic Cloud. I.
  Constraints on the Star Formation History in Different Fields
OLD MAIN-SEQUENCE TURNOFF PHOTOMETRY IN THE
SMALL MAGELLANIC CLOUD. I. CONSTRAINTS ON THE
STAR FORMATION HISTORY IN DIFFERENT FIELDS
Noelia E. D. Noël
Instituto de Astrof́ısica de Canarias. 38200 La Laguna. Tenerife, Canary Islands. Spain.
noelia@iac.es
Carme Gallart
Instituto de Astrof́ısica de Canarias. 38200 La Laguna. Tenerife, Canary Islands. Spain.
carme@iac.es
Edgardo Costa
Departamento de Astronomı́a, Universidad de Chile, Casilla 36-D, Santiago, Chile.
costa@das.uchile.cl
René A. Méndez
Departamento de Astronomı́a, Universidad de Chile, Casilla 36-D, Santiago, Chile.
rmendez@das.uchile.cl
ABSTRACT
We present ground-based B and R-band color-magnitude diagrams (CMDs),
reaching the oldest main-sequence turnoffs with good photometric accuracy for
twelve fields in the Small Magellanic Cloud (SMC). Our fields, located between
∼1◦ and ∼4◦ from the center of the galaxy, are situated in different parts of the
SMC such as the “Wing” area, and towards the West and South. In this paper
we perform a first analysis of the stellar content in our SMC fields through com-
parison with theoretical isochrones and color functions (CFs). We find that the
underlying spheroidally distributed population is composed of both intermediate-
age and old stars and that its age composition does not show strong galacto-
centric gradients. The three fields situated toward the east, in the Wing region,
http://arxiv.org/abs/0704.1151v1
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show very active current star formation. However, only in the eastern field closest
to the center do we find an enhancement of recent star formation with respect
to a constant SFR(t). The fields corresponding to the western side of the SMC
present a much less populated young MS, and the CF analysis indicates that
the SFR(t) greatly diminished around 2 Gyr ago in these parts. Field smc0057,
the closest to the center of the galaxy and located in the southern part, shows
recent star formation, while the rest of the southern fields present few bright MS
stars. The structure of the red clump in all the CMDs is consistent with the large
amount of intermediate-age stars inferred from the CMDs and color functions.
None of the SMC fields presented here are dominated by old stellar populations,
a fact that is in agreement with the lack of a conspicuous horizontal branch in
all these SMC CMDs. This could indicate that a disk population is ruling over
a possible old halo in all the observed fields.
Subject headings: local group galaxies: evolution — galaxies: individual (Small
Magellanic Cloud) — galaxies: photometry — galaxies: stellar content — Local
Group
1. INTRODUCTION
Dwarf galaxies are believed to represent the dominant population, by number, of the
present day universe, and a major constituent of groups (Côté et al. 1997) and clusters (e.g.
Ferguson & Sandage 1991). Studying their star formation and chemical enrichment histories
is key to understanding the evolution of galaxies on cosmological timescales (e.g. Madau et
al. 1998). Local Group galaxies are ideal laboratories for detailed studies of dwarf galaxy
properties: we can resolve their individual stars and thus learn about their star formation
histories (SFHs) by exploring ages, metallicities, and the spatial distribution of the stellar
populations they contain.
The color-magnitude diagram (CMD) is the best tool to retrieve the SFH of a stellar
system. The ideal situation is when it reaches the oldest main-sequence (MS) turnoffs with
good photometric accuracy. In this case, the information on the SFH can be obtained directly
and with little ambiguity from the distribution of stars on the MS, and its comparison with
that predicted by stellar evolution models in this relatively well known phase of stellar
evolution. In particular, the range of ages and metallicities present can be determined
through comparison with theoretical isochrones. To quantitatively determine the SFH, it
is necessary to compare the observed density distribution of stars with that predicted by
stellar evolution models (see Gallart, Zoccali & Aparicio 2005). Shallower CMDs (e.g. those
– 3 –
reaching just below the horizontal-branch (HB) or a couple of magnitudes below the tip of
the red giant branch (RGB)) still contain stars born through the whole galaxy’s lifetime,
but the interpretation of the distribution of stars in terms of the SFH is progressively less
detailed and uncertain as the CMD is shallower. The reason for this is twofold: on one hand,
the stellar evolution models are less accurate for more advanced stellar evolution phases such
as the RGB or the HB, because the corresponding physics is more complicated or uncertain.
On the other hand, in these stellar evolution phases, stars of very different ages are packed
together in the CMD in a small interval of color and/or magnitude, and suffer from important
age-metallicity degeneracies (see Gallart 2000 and Gallart et al. 2005 for detailed discussions
of all these issues).
For all the Milky Way satellites, it is possible to obtain CMDs reaching the oldest MS
turnoffs using ground based telescopes, while for the rest of the Local Group, this is possible
using the ACS on board the HST. The Magellanic Clouds (MCs) are particularly interesting
among the Milky Way satellites since they are actively star forming galaxies which SFH
can shed light on the role played by interactions in galaxy evolution. But in spite of their
proximity and intrinsic interest, it is remarkable that there are still important gaps in the
knowledge of the SFH of the MCs. This may be explained by their huge projected size and
the big number of stars to analyze.
In this paper we will focus on the Small Magellanic Cloud (SMC). The SMC is a dwarf
irregular satellite of our Galaxy, with low mean metallicity and a high mass fraction remain-
ing in gaseous form (van den Bergh 1999). These characteristics suggest that the SMC is
in a more primitive evolutionary stage than its larger neighbor, the Large Magellanic Cloud
(LMC). Historically, the study of this galaxy has been in general neglected in favor of the
LMC. The uncertainty about its line of sight depth, its more complicated shape (elongated
towards the Northeast), and its larger distance from us are factors at play.
To our knowledge, only two papers have presented CMDs reaching the oldest MS turnoffs
for a small field of view each: Dolphin et al. (2001) and McCumber et al. (2005). Dolphin
et al. presented a combination of HST and ground-based V and I images of a SMC field
situated 2◦ Northeast of NGC 121 (avoiding the contamination from 47 Tucanae) in order to
derive the SFH of this SMC field. From their ground-based images, they inferred a peak of
star formation between 5 and 8 Gyr ago with a medium age of 7.5 Gyr at the 1 σ level, and
that 14±5% of the stars were formed more than 11 Gyr ago. The SFH they derived is also
consistent at the 2 σ level with a continuous star formation from ancient times until ∼2 Gyr
ago, when the star formation rate dropped to finally stop entirely in the past 0.5 Gyr. More
recently, McCumber et al. (2005) analyzed the stellar populations of a SMC field located in
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the “Wing”1 area with observations from the HST WFPC2. They compared the luminosity
function from their observed CMD with those obtained from two different model CMDs, one
with constant SFR(t) and another with bursts of star formation at ∼2 and at ∼8 Gyr. They
found that the population appears to have formed largely in a quasi-continuous mode, with
a main period of star formation between 4-12 Gyr ago and very recent star formation with
bright stars as young as 100±10 Myr.
Two main wide field studies of the SMC exist: the pioneer work by Gardiner & Hatzidim-
itriou (1992) and a recent study from Harris & Zaritsky (2004; hereafter HZ04). Gardiner
& Hatzidimitriou (1992) presented the first large area study of the SMC, and mainly con-
centrated their analysis in the outer regions, beyond 2◦ from the SMC center. They took
six photographic plates with the UK Schmidt Telescope covering a total area of 130◦×130◦.
Since their photometry is rather shallow (reaching the HB level at R∼20 mag), they mainly
gave information about the young populations (age ≤2 Gyr). From their CMDs and con-
tour plots of the surface distribution of MS stars with B-R<0.1 and R<20, they noticed the
almost complete absence of bright MS stars in the Northwestern part, while a considerable
bright MS population was present in the Eastern and Southern area. With the aid of lu-
minosity functions they found that young populations (<0.6 Gyr in age) are concentrated
towards the center of the SMC and in the “Wing” region. Using an index defined as the
difference between the median color (in (B-R)) of the RC and the color of the RGB at the
level of the HB, the authors inferred that the bulk of the field population has a median age
around 10-12 Gyr. They were the first to notice the different distribution of young and old
populations in the SMC. Zaritsky et al. (2000) and Cioni et al. (2000) confirmed that the
asymmetric appearance of the SMC, similar to that of the HI (Stanimirović et al. 1999),
is primarily caused by the distribution of young stars (upper MS stars, younger than ∼0.2
Gyr), and that the older stars have a spheroidal distribution.
HZ04 presented a study of the SMC based on the Magellanic Clouds Photometric Survey
(MCPS) UBVI catalog (Zaritsky et al. 1997), which covers a 4◦×4.5◦ area of the SMC to
a depth of V≤21. This work represents the most complete analysis of the spatially resolved
SFH of the central part of the SMC. They divided the SMC survey in a grid of 351 cells
and obtained the SFH, through a χ2 minimization between the star counts in the observed
CMD and those in the model CMDs based on isochrones by Girardi et al. (2002). They
inferred that a significant fraction (∼50%) of all stars in the SMC were formed more than
8.4 Gyr ago. Between 3 and 8.4 Gyr ago they found a quiescent period during which the
1We call “Wing” area to the Eastern part of the SMC. Some authors (in particular, Gardiner & Hatzidim-
itriou (1992) and papers in the same series) also distinguish between the inner and outer “Wing” and the
“Arm”.
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SMC formed few stars. They also found a recent active time from 3 Gyr ago until now,
with bursts at 2.5 Gyr, 400 Myr, and 60 Myr. Although deeper than the one from Gardiner
& Hatzidimitriou (1992), this study is still limited by its shallowness. In fact, the oldest
stars that they can observe on the MS are ∼2 Gyr old, and this implies a necessarily poor
temporal resolution and larger uncertainties in their SFH at ages older than that.
In spite of the increasing interest in studying the SMC, reflected by the recent works
mentioned before, there are still many questions unanswered which require the information
provided by CMDs reaching the oldest MS turnoffs. What is the age distribution of the old
and intermediate-age population?, are there gradients in the composition of this underlying
population?. Shallower studies inform about the existence of a large amount of young popu-
lation in certain areas, but does this young population reflect an exceptional increase of the
star formation at the present time with respect to the average SFR?. To shed light on these
aspects, in this article we present twelve unprecedented deep BR-based SMC CMDs with
positions ranging from ∼1◦ to ∼4◦ from the SMC center. Our fields are distributed in differ-
ent parts of the SMC, avoiding the central area, where crowding may not allow us to reach
the oldest MS turnoffs from the ground. Three of our fields are located in the “Wing” area,
near the field studied by McCumber et al. (2005); two fields are in the Western part and one
in the Northwestern area, near the field from Dolphin et al. (2001) located 2◦ northeast of
NGC121; finally, six fields are placed towards the South at different galactocentric distances.
This strategic selection of fields, in spite of their small size, permit us to sample several
regions of the SMC with high temporal resolution in order to address the above issues. The
depth of our fields, reaching the oldest MS turnoffs with very good photometric accuracy,
will allow us to obtain detailed SFHs from all of them, and to investigate, therefore, the
variation of the SFH across the SMC field. This will be the subject of a forthcoming paper.
Here we will focus the analysis in the inspection of the CMDs with the aid of theoretical
isochrones and color functions.
This paper is organized as follows. In § 2 we present the observations and data reduction.
In § 3 we discuss the photometry of the SMC fields, obtained using DAOPHOT II/ALLSTAR
and ALLFRAME programs. In § 4 the CMDs are discussed with the help of isochrones and
color functions. In § 5 and § 6 our results are summarized and discussed. In a future paper
(Noël et al., in preparation) we will derive the SFH of the SMC through comparison of the
observed CMDs with synthetic CMDs.
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2. OBSERVATIONS AND DATA REDUCTION
The present paper is a result of a more comprehensive program to study the SMC, which
also includes the determination of its Absolute Proper Motion by observing SMC fields in
which background quasars have been identified. These quasars provide a quasi-inertial refer-
ence frame with respect to which (in conjunction with existing radial velocity measurements)
the absolute total space velocity vector of the SMC can be precisely determined (see e.g.
Pedreros, Costa & Méndez 2006). The imaging strategy was therefore designed in a way
that would satisfy the needs of the stellar populations program as well as the astrometry
program. Given that for the latter it was mandatory to obtain R-band images, this bandpass
together with B imaging was chosen to construct the CMDs.
The observations were made with a 24 µm/pixel Tektronic 2048x2048 CCD detector
attached to the Cassegrain focus of the 100-inch Irénée du Pont telescope (C100) at Las
Campanas Observatory, in Chile. This combination gives a field size of 8.85′×8.85′ and a
scale of 0.259′′/pixel. Inverse gain was 3e−/ADU with a read noise of 7e−. Basic reduction
of the CCD frames was done using standard IRAF2 tasks. For this purpose, bias exposures,
sky flats, and dome flats were taken every night.
Throughout our four year campaign (2001-2004), B and R band images of thirteen
fields in the SMC were obtained. The coordinates of these fields and the data obtained for
each of them are detailed in Table 1, where the first column denotes the field, the second
and third columns the right ascension and the declination respectively, fourth and fifth
columns the galactocentric distance (r) and the position angle (p), and the sixth and seventh
columns the integration times in B and R. Seeing was typically between 0.′′7 and 1.′′2 in all
epochs. Figure 1a shows a HI column-density image of the SMC taken from Stanimirović
et al. (1999) with our SMC fields (black squares) and the fields from Dolphin et al. (2001)
and McCumber et al. (2005) (black circles) overlapped. The black rectangle denotes the
area covered by the MCPS (Zaristky et al. 1997). The actual figure from Stanimirović et
al. (1999) includes the range in declination from ∼-75◦ to ∼-70◦. Those squares denoted
with “qj” represent the fields centered in quasars observed for astrometric purposes. We
followed the naming convention by Tinney et al. (1997), in which the numbers following
“qj” refer to the right ascension of the quasar (the declination, includded in the full Tinney
naming convention, was ommitted). The fields denoted with “smc” (and followed by the
right ascension, for consistency with the naming convention) were specifically selected for
this project and were chosen to span a wide range of galactocentric distances, from ∼1◦ to
∼4◦. The combination of “qj” and “smc” fields results in a sampling of the SMC that covers
2version 2.11.3, NOAO, University of Arizona
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Fig. 1.— Panel (a) shows the spatial distribution of our SMC fields (black squares) over-
lapped on an HI column-density image of the SMC from Stanimirović et al. (1999). The big
rectangle denotes the area covered by the MCPS (Zaritsky et al. 1997). The position of the
fields studied by Dolphin et al. (2001) and McCumber et al. (2005) is also superimposed.
The actual figure from Stanimirović et al. (1999) is delimitated by the labelled box and
includes the range in declination from ∼-75◦ to ∼-70◦. The grey-scale intensity range is 0
to 1.03×1022 atom/cm2 with a linear transfer function. The maximum HI column-density
is 1.43×1022 atom/cm2. Panels (b) and (c), are taken from Cioni et al. (2000), and show
the distribution of young and RGB stars in the SMC respectively. The position of our fields
has also been overlapped. The fields superimposed are the same in the three figures but the
name of each field in panels (b) and (c) have been omitted for clarity.
– 8 –
both a good range of galactocentric distances and position angles. It is important to note
that given the elongation of the SMC, with a position angle of ∼45◦ (Cioni et al. 2000), a
certain galactocentric distance in the Northwest or Southeast directions is different than in
the Southwest or Northeast directions in which the stellar densities are larger. Figure 1b
show the distribution of young MS stars and Figure 1c the layout of the RGB (intermediate-
age and old population) stars in the SMC from Cioni et al. (2000) with our SMC fields
superimposed. The name of each field was omitted for clarity.
3. THE PHOTOMETRY
3.1. Photometry of SMC fields
We performed our photometry using the DAOPHOT II/ALLSTAR software package
(Stetson 1987, and updates: Stetson 1990, 1992) to find stars and to determine an empirical
PSF for each frame and then simultaneously fit it to all detected stars. After testing various
PSF models, we adopted a Moffat function with β=2.5 (Stetson et al. 2003) as the best
analytical model. The Moffat function is usually a much better representation of a star
image than a Gaussian function, because it has more prominent and extended wings, like
real star images. Also, unlike other functions (e.g. the Lorentz function), the Moffat function
offers the option of tuning the radial falloff of the wings to match observations. Between 50
and 100 stars were used to construct the PSF of each image. Quadratic spatial variation
was included because it reduced the fitting errors.
After the DAOPHOT/ALLSTAR analysis of all the original frames was performed, an
optimum, complete star list was achieved by cross matching the ALLSTAR results of the
individual frames with DAOMASTER (Stetson 1993). ALLFRAME (Stetson 1994) was then
used to obtain simultaneous photometry of stars in all CCD images of each SMC field.
After ALLFRAME, we ran MONTAGE2 for each field. MONTAGE2 takes the images
from which all the stars have been subtracted according to their final positions and bright-
nesses, and applies the known geometric transformations that relate their coordinate systems
and the known differences in their photometric zero-points, to produce a median image of
each field. We tested in each of the 13 SMC fields that the number of stars detected on
the median of the subtracted images, and considered real stars after running DAOPHOT,
ALLSTAR, and ALLFRAME a second time, was less than 1%, i.e. negligible for our goal.
ALLFRAME produces an image-quality index, CHI, which is a dimensionless measure
of the agreement between the brightness profile of any given object and that of the model
PSF for the frame in which it is measured. Similarly, ALLFRAME gives the SHARP index,
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which is a first-order estimate of the intrinsic angular radius of a source. Another index
provided by ALLFRAME is σ, which represent the standard error of the star’s magnitude
and is representative of the internal errors of the photometry. Stars with at least one valid
measurement in each band (B and R) were selected, and their final magnitudes were obtained
using DAOMASTER, which combines the magnitudes measured for each star in each image
to provide the “mean weighted” magnitude. DAOMASTER also provides σ, CHI, and
SHARP parameters for each stars, which are a combination of the corresponding parameters
for each image. We used the following limits for the error and shape parameters given
by DAOMASTER: σ(B−R)
260.15, -0.66|SHARP|60.6, and |CHI|62.5. The final
number of stars we kept, measured in (B-R) of each field (and consequently, in each CMD)
is given in Table 2. A total of 215,121 stars down to R≈24 were measured.
The so-called aperture corrections, i.e., the corrections that place the relative profile-
fitting magnitudes on the system of the “total” instrumental magnitudes for a particular
frame, were obtained from synthetic aperture photometry by measuring several isolated,
bright stars through a series of increasing apertures and the construction of growth curves
(Stetson 1990). We used a growth sequence which consists in twelve apertures from r1 to
r12 in such a way that we considered the first radius r1 about half of the one we used for
the aperture photometry of our objects and r12=30
′′. The sequence is rk=
r12/r1× rk−1 ,
k = 2, ..., 12. The aperture corrections were derived using the program DAOGROW (Stetson
1990). In each image we selected the brightest and most isolated 30 to 80 stars among those
used in the derivation of the PSF for that frame. The aperture photometry results were
then provided to DAOGROW which returns the “total” instrumental magnitude and its
standard error for each of the selected stars. The aperture correction for a particular frame
was obtained as the median of the differences between the “total” magnitude and the profile-
fitting ALLFRAME magnitude for all selected stars on that frame. Errors in the aperture
corrections were calculated as the standard error of the mean of these differences, and were
typically between ±0.001 and ±0.003.
3.2. Standard Stars Photometry
Our instrumental photometric system was defined by the use of the Harris BVRI filter
set, which constitutes the default option on the C100 for broad-band photometry on the
standard Johnson-Kron-Cousins system. In photometric nights, typically six BVRI standard
star areas from the catalog of Landolt (1992) were observed several times to determine the
transformation of our instrumental magnitudes to the standard BR system. Thirty-one
different standard stars with colors: -0.49<(B-R)<5.00 were observed, and a total of 272
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Table 1. Data obtained in the SMC
Field α2000 δ2000 r(
′)a p(◦) B-band exposures (sec) R-band exposures (sec)
smc0057 00:57 -73:53 65.7 164.4 1×60+1×600+2×800+2×1000+1×1200 2×60+2×600+3×800+1×1200
qj0037 00:37 -72:18 78.5 294 1×60+5×800 7×60+16×600
qj0036 00:36 -72:25 79.8 288 2×60+10×600+12×800 15×60+26×500+22×600
qj0111 01:11 -72:49 80.9 89.5 1×60+3×800 8×60+4×500+17×600+1×700+1×800
qj0112 01:12 -72:36 87.4 81 1×60+1×600+6×800 9×60+7×500+15×600
qj0035 00:35 -72:01 95.5 300.6 4×600+1×700 4×60+1×100+3×500+15×600+3×800
qj0116 01:16 -72:59 102.5 95.2 1×60+13×600+2×800 7×60+14×500+20×600
smc0100 01:00 -74:57 130.4 167.5 1×60+7×800+3×900 1×60+7×600+3×700
qj0047 00:47 -75:30 161.7 187.7 1×800+3×1000 6×60+16×600+2×800
qj0033 00:33 -70:28 172.9 325 1×60+5×600+1×700 6×60+3×500+20×600
smc0049 00:49 -75:44 174.8 184.6 1×60+1×600+4×800 1×60+5×600
qj0102 01:02 -75:46 179.5 169.4 3×60+6×800 8×60+3×500+15×600+1×700+2×800
smc0053 00:53 -76:46 236.3 179.4 1×60+8×800+2×900 1×60+8×600+2×700
aDistance from the SMC center, α2000 = 00:52.7, δ2000 = -72:49
Table 2. Final number of stars measured in (B-R)
Field N†
smc0057 21246
qj0037 21579
qj0036 23756
qj0111 25845
qj0112 47548
qj0035 24114
qj0116 19875
smc0100 7801
qj0047 9762
qj0033 3797
smc0049 3580
qj0102 4030
smc0053 2188
†Selected stars with σ60.15,
CHI62.5 and -0.66SHARP60.6.
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observations were made; 178 in 2001 and 94 in 2002. Most of these areas include stars of a
wide variety of colors. A few of them were followed up to about 2.0 airmasses to determine
atmospheric extinction optimally. During these nights we also obtained short exposure BR
frames of all our fields of interest, which served the purpose of calibrating all frames taken
with non-photometric sky. Field qj0035 is not considered in this paper because we do not
have yet a secure calibration for it.
The Landolt standard images are uncrowded fields, thus no profile-fitting photometry
was necessary for them. Instead, DAOGROWwas used in an identical way as for the program
stars to directly derive the total instrumental magnitudes for the standard stars from their
aperture photometry.
To put our observations into the standard system, we used the following transformation
equations:
B = b+ αb + βb(B −R) + γbXb
R = r + αr + βr(B −R) + γrXr
where (b, r) and (B,R) are the instrumental and standard magnitudes respectively, and
(Xb, Xr) are the airmasses. No time dependence terms were added since a preliminary fit
showed no trends in the residuals of both B and R with time.
The color terms (βb, βr) and extinction coefficients (γb, γr), as well as the zero-points (αb,
αr) are unknown, presumably constant, transformation coefficients and are to be calculated.
Both the color-dependent term and the zero-point in the transformation, are expected to
be reasonably constant properties of the telescope/filter/detector combination and, in fact,
the night-to-night differences for a given year in their computed values were found to be
consistent with the uncertainty of the individual determinations. The above equations were
applied to the Landolt standard star magnitudes, and solved for αb, αr, βb, βr, γb and γr,
for each night, using a custom program.
Then, we followed an iterative procedure to refine our photometric transformation.
First, a new set of unique (αb, αr) and (βb, βr) values for each campaign was obtained by
imposing the extinction coefficients (γb, γr) corresponding to each night. Then, we applied
the resultant zero-points and color terms to each night of each year and new extinction
coefficients were derived for each night. In this way, we have a set of (αb, αr) and (βb, βr)
values for each year and (γb, γr) values for each night of each year. In Table 3 we present
the zero-points and the color coefficients. The first column denotes the year, the second
– 12 –
and third columns indicate the (αb, αr) coefficients, and fourth and fifth columns the (βb,
βr) coefficients. The final values for the extinction coefficients are shown in the second and
third columns of Table 4, where the first column shows the night to which the coefficients
correspond. Figure 2 shows the standard distributions for each filter and each year; the
slope represents the extinction coefficient. Fitting errors in the zero-points correspond to
(N − 2), where N is the number of measurements we have. They turned out to be
between ±0.001 and ±0.002.
The total zero-point errors of the photometry, including the error in the extinction, in
the aperture corrections, and the uncertainties in the calibrations, are ∼0.02 mag in both B
and R. These values are consistent with the systematic errors derived comparing photometry
of different epochs. Using those SMC fields for which we have standard star observations
from more than one night, we tested the photometric differences resulting from the use of
different standard sets corresponding to different nights. We found that these differences are
between ±0.001 and ±0.03 in B and between ±0.001 and ±0.04 in R (standard errors of the
mean).
4. THE SMC STELLAR CONTENT
We present unprecedented deep SMC CMDs obtained using a medium aperture telescope
(100-inch). The quality of the CMDs is comparable to that of the CMDs obtained for the
MCs using the HST (e.g. McCumber et al. 2005). Given the depth of our diagrams, which
reach the oldest turnoffs, accurate information about age can be derived from the MS turnoff
luminosities. As discussed by Gallart, Zoccali, & Aparicio (2005), reaching the oldest turnoffs
will allow us to break the age-metallicity degeneracy affecting most methods to obtain the
Figures 3 to 5 show the [(B-R),R] CMDs for the twelve SMC fields in order of increasing
galactocentric distance. The fields range from galactocentric radius ∼1◦ to ∼4◦, and sample
different regions of the SMC, as shown in Figure 1, where the fields are depicted in the context
Table 3. Transformation equation coefficients
Campaign αb αr βb βr
2001 -0.709±0.002 -0.423±0.001 +0.040±0.002 +0.001±0.001
2002 -0.892±0.002 -0.549±0.002 +0.045±0.002 +0.002±0.002
– 13 –
1 1.5 2 2.5
std2002B
1 1.5 2 2.5
std2001B
1 1.5 2 2.5
std2001R
1 1.5 2 2.5
std2002R
Fig. 2.— The upper panels show the [B-b-βb(B-R)] vs. Xb (for standards in B-band)
and the lower panels show the [R-r-βr(B-R)] vs. Xr (standards in R-band) for 2001 and
2002. The slope correspond to the extinction coefficient value. Open triangles correspond to
10/16/2001, open squares to 10/17/2001, diagonal crosses to 10/18/2001 and open circles
to 10/19/2001. For 2002, open squares correspond to 10/10 and filled triangles to 10/13.
– 14 –
Fig. 3.— CMDs corresponding to the fields on the Eastern side of the SMC, in order of
increasing distance from the SMC center (r) and with different position angles (p).
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Fig. 4.— CMDs corresponding to the Western side of the SMC, in order of increasing
distance from the SMC center (r) and for different position angles (p).
– 16 –
Fig. 5.— CMDs corresponding to the Southern side of the SMC, in order of increasing
distance from the SMC center (r) with different position angles (p).
– 17 –
of the HI distribution (Figure 1a), and of the young (Figure 1b) and intermediate-age and
old (RGB stars) populations (Figure 1c). All the CMDs reach a couple of magnitudes below
the old MS turnoff (even the most populated), with great photometric accuracy.
Figure 3 shows the CMD of fields qj0111, qj0112, and qj0116, which have a galactocentric
radius ranging from 1.4◦ to 1.7◦. These fields correspond to the Eastern side of the galaxy
(facing the LMC) as seen in Figure 1a, from which we can notice that they are located in
an area of high HI concentration, inside the Supergiant Shell 304A with HI mass of 5.7×107
M⊙ (the total HI mass in the area observed by Stanimirović et al. is ∼4×10
8 M⊙). These
fields are also in the region of the bridge which connects the so-called “stellar bar”3 with the
“Wing”. From Figure 1b and Figure 1c, it can be noticed that these fields are located in
very densely populated isopleths of young, intermediate-age and old population. Indeed, the
CMDs of these fields show a conspicuous MS, well populated from the oldest turnoff at R∼22
to R∼16, which implies the presence of a large number of very young stars in all the CMDs.
The three Western fields are also shown in Figure 1a and the corresponding CMDs are
presented in order of increasing galactocentric distance from 1.3◦ to 2.9◦ in Figure 4. These
fields are situated in the opposite side of the LMC, in a region with low concentration of HI.
From Figure 1b it is evident that they are located in an area of low young stellar density,
but still high density of intermediate and old population similar to that of the Eastern fields.
The CMDs of these Western fields show a less significant MS, even at similar distances from
the center as the Eastern fields. This fact is in agreement with the low density of the HI
column in this part of the galaxy (see Figure 1a). We would like to address if the differences
seen in the young population can be extended to the intermediate and old population.
Figure 5 shows the CMDs of the six Southern fields, whose galactocentric distances
3The SMC is not a type of barred Irr galaxy, for which the LMC is the prototype, but sometimes it is
useful to call bar to the brightest portion of its chaotic major axis.
Table 4. Atmospheric extinction coefficients
Night γb γr
16/10/2001 -0.218±0.007 -0.078±0.003
17/10/2001 -0.219±0.007 -0.077±0.007
18/10/2001 -0.219±0.006 -0.070±0.009
19/10/2001 -0.211±0.005 -0.065±0.005
10/10/2002 -0.207±0.008 -0.066±0.009
13/10/2002 -0.215±0.008 -0.076±0.008
– 18 –
range from 1.1◦ to 4◦. As seen in Figure 1a these fields are located in regions in which the HI
column-density is very low. Field smc0057, the closest to the center, presents a conspicuous
young MS. In Figure 1b is shown that the stellar density of young stars in this field is higher
than in the rest of the Southern fields and similar to the Eastern field qj0111. Field smc0100
still shows many bright young MS stars but further on 2.7◦ the CMDs have less populated
young MS, and present a similar distribution of stars (with less statistics while going further
South). The four furthest fields are located in an area in which the stellar density is similar,
as shown in Figures 1b and 1c.
Depending on their mass and metallicity, the core He-burning stars produce the horizon-
tal branch (HB) and the RC. The presence of a prominent blue HB points out the existence
of an old, metal poor population; the lack of such HB and the presence of a RC may indicate
that core He burners are not so old, or more metal rich, or both (see Gallart et al. 2005
for details). A shared feature in all our SMC CMDs is the absence of a well populated,
blue extended HB, pointing out that the amount of field stellar population as old and metal
poor as that of the Milky Way halo globular clusters and dwarf spheroidal galaxies is small
in the SMC. The RC is well populated and extended in luminosity, with a width of up to
△R∼1 mag, denoting the presence of a large intermediate-age population. The fields with
a prominent bright MS, as the Eastern fields and smc0057, for example, show the vertical
extension of the RC feature corresponding to non-degenerate core He-burners (Gallart 1998).
The older stars in the core He-burning phase lie in the lower part of the observed RC, while
younger stars are brighter.
In the following sections, we discuss the main features of the SMC CMDs using isochrones
(sec § 4.1) and Color Functions (sec § 4.2). This will allow us to describe the SMC stellar
populations, as a starting point to a study (Noël et al., in preparation) in which we will ad-
dress the SMC SFH by comparing in detail the distribution of stars in the observed CMDs
with a set of model CMDs.
4.1. Theoretical isochrones
The interpretation of CMDs of composite stellar population strongly relies on the stellar
evolution models adopted (see Gallart et al. 2005). For the present work, we used the
Teramo stellar evolution models (Pietrinferni et al. 2004) as the reference. In Figures 6, 7,
and 8 we have superimposed Teramo isochrones to our CMDs for three different metallicities
suitable for the SMC stellar populations: Z=0.001 ([Fe/H]=-1.27), Z=0.002 ([Fe/H]=-0.96),
and Z=0.004 ([Fe/H]=-0.66). The final selection of the metallicities was done taking into
account the RGB and MS star colors and its best match by Teramo isochrones of given ages
– 19 –
and metallicities.
The observed CMDs have been transformed to absolute magnitudes using a distance
modulus of (m − M)0 = 18.9 (see van den Bergh 1999) and de-reddened as follows. For
the two outermost fields, the reddening values given by the IRAS/COBE extinction maps
(Schlegel, Finkbeiner & Davis 1998) were used. For the innermost regions, Schlegel et al.
(1998) estimate a typical reddening of E(B-V)=0.037, from the median dust emission in
surrounding annuli, since reddenings through the SMC cannot be calculated because its tem-
perature structure is not sufficiently well resolved by DIRBE. Their quoted value, therefore,
is not accurate enough and we have estimated a mean value of the reddening for each of the
fields smc0057, qj0037, qj0036, and qj0111 by requiring a good fit of the CMD by the same
isochrones that were overlapped to the other fields, for which the IRAS/COBE reddening
values are reliable. This assumes the same age-metallicity relation for all fields, which is in
agreement with the results found by Carrera (2006) and Carrera et al. (2006, in preparation)
using CaII triplet spectroscopy.
In all cases, the relations AB = 1.316E(B-V), and AR = 0.758 E(B-V) (Schlegel et al.
1998) have been assumed to calculate the extinction in the B and R bands.
Canonical isochrones of 6, 9, and 13 Gyr with Z=0.001, isochrones with overshooting of
1, 3, and 4 Gyr with Z=0.002, and of 0.1 Gyr with Z=0.004 were overlapped. In the Eastern
fields and in field smc0057 a 0.03 Gyr isochrone with overshooting and Z=0.004 was also
superimposed.
Figure 6 shows the CMDs of the Eastern fields with the superposition of Teramo
isochrones. In these CMDs the conspicuous MS is well populated from the oldest turnoff
at MR=3.5 (13 Gyr isochrone) up to the 0.03 Gyr isochrone. All the CMDs show a large
number of young stars well represented by the 0.03 Gyr and 0.1 Gyr isochrones. The areas
around the 1 to 6 Gyr isochrones are densely populated, indicating a strong presence of
intermediate-age stars. No obvious differences between the MS of these fields can be inferred
from the comparison with isochrones alone.
Figure 7 shows the CMDs of the Western fields with the isochrones overlapped. In these
fields, the intermediate-age population (∼3-4 to 9 Gyr) seems dominant. Fields qj0036 and
qj0037 have a small fraction of stars born up to 0.1 Gyr ago, while qj0033, the most remote
of the three, seems to have no stars younger than 1 Gyr (though this could be an effect of
small number statistics).
Figure 8 shows the CMDs of the six Southern fields with the superposition of isochrones.
Field smc0057, the closest to the center, presents an important MS where the 0.1 Gyr
isochrone is still quite populated. In field smc0100 there is still a substantial population
– 20 –
Fig. 6.— Fields located to the East side of the SMC, with Teramo isochrones (Pietrinferni
et al. 2004) superimposed. The CMDs were transformed to absolute magnitudes using (m-
M)0=18.9, and de-reddened with the reddening labelled, obtained using the criteria explained
in the text.
– 21 –
Fig. 7.— As in Figure 6, but showing the CMDs of fields located to the West side of the
– 22 –
Fig. 8.— As in Figure 6, but showing the CMDs of fields located to the South of the SMC.
– 23 –
between 1 and 3 Gyr old, but fields qj0047 to smc0053 show few stars younger than 3-4 Gyr.
The population of these relatively far-off fields is not purely old but contains an important
amount of intermediate-age stars that inhabit the zones of the MS and subgiant branch
around the 3, 4, 6, and 9 Gyr isochrones, in addition to the several old stars around the 13
Gyr isochrones.
4.2. Color Functions
Gallart et al. (2005) have discussed the potential of MS Color Functions (CFs) to
provide information on the stellar populations present in a galaxy. They concluded that, in
fact, the CF may be a better tracer of the SFH than the LF. The reason is that, in CMDs
like [(B-R), R] or [(V-I), I], the MS of isochrones of different age follow roughly vertical
paths up to the MS turnoff where they turn to the red, almost perpendicularly to the MS,
to form the subgiant branch or, in the case of more massive stars, the blue loops. This
effect is clear from the CMD in panel (a) of Figure 9 (we will return to this figure later).
The fact that the turnoff of a stellar population gets redder as the populations gets older
implies a general dependency on age of the CF of the MS and subgiant branch stars brighter
than the oldest MS turnoff. Here we will discuss CFs that will include the whole CMD
within a region comprised between: -16MR63.5 and -0.56(B-R)61.5. The star counts have
been normalized to the total stars present in the integrated range. Most of the information
belongs in any case to the MS and subgiant branch. The fraction of CF that belongs to
the RGB and RC serves as a check of the metallicity assumed for the synthetic CMD, and
contributes to the overall normalization of the CF.
Comparison of the stellar content of a galaxy with isochrones and CFs is complementary
in terms of the information on the stellar population they provide. The isochrones give us
the range of ages present in a given CMD; the comparison between theoretical and observed
CFs is a good tool to assess the relative amounts of stars of different ages present in a stellar
population. This is a particular case of a comparison of the number of stars in a set of boxes
in the observed and synthetic CMDs respectively (e.g. Gallart et al. 1999). However, the
CF is particularly useful for a first qualitative assessment of the SFH because it is a one-
dimensional representation of the content of the CMD in which there is a relatively direct
correlation between range of ages and color. All the models used here have been computed
using the synthetic CMD algorithm iac-STAR (Aparicio & Gallart 2004).
Panel (a) in Figure 9 shows a synthetic CMD calculated assuming a constant SFR(t)
from 13 Gyr ago to date and metallicities: Z=0.004 in the range 0 Gyr6t61 Gyr, Z=0.002
in the range 1 Gyr6t65 Gyr, and Z=0.001 in the range 5 Gyr6t613 Gyr (see inset). Stars
– 24 –
Fig. 9.— The panel (a) shows a synthetic CMD showing the position of stars in different ages
intervals. The Teramo stellar evolution models have been used in the computation using the tool iac-
STAR (http://iac-star.iac.es/iac-star/). Constant SFR(t) from 13 Gyr ago to the present time has
been assumed. In the inset on top of panel (a) the metallicity law used is shown: Z=0.004 ([Fe/H]=-
0.66) between 0 and 1 Gyr ago, Z=0.002([Fe/H]=-0.96) between 1 and 5 Gyr ago, and Z=0.001
([Fe/H]=-1.27) between 5 and 13 Gyr ago. In panel (b) different CF distributions, corresponding to
synthetic populations with different SFR(t) and integrated in the range -1<MR<3.5 are depicted
(see inset). Black CF correspond to the CMD in panel (a). The CF for a population with an
enhancement in the SFR(t) 3 Gyr ago is depicted in blue. The green CF represents a population in
which the SFR(t) decreased by 50% between 8 and 3 Gyr ago. The CF in red represents a population
with a gap in the SFR(t) between 8 and 3 Gyr ago. Panel (c) shows the CF corresponding to the
CMD in panel (a) with limited age ranges, as described in the labels.
http://iac-star.iac.es/iac-star/
– 25 –
corresponding to each age interval are depicted in different colors. A 30% of binary stars
have been assumed; the parallel feature to the red of the MS between 3.56MR65 corresponds
to binary stars. Some of these binaries between 8-13 Gyr old are noticeably brighter than
single stars at the same age and mass (red points in the synthetic CMD between 26MR63).
Panel (b) in Figure 9 shows the composite CFs of populations with different SFR(t)
(shown in the inset). Three main features characterize the CF: a local elevation in the blue
part between -0.36(B-R)60.2, a central peak between 0.26(B-R)60.9, and a second local
maximum in the red part. Panel (c) of Figure 9 shows which populations contribute to each
feature in the CF for the synthetic CMD in panel (a). By comparing these, we find the
following: the elevation in -0.3.(B-R).0.2 in the composite CF mostly corresponds to stars
in the age range 06t.1.1 Gyr; in the central peak (0.3.(B-R).0.9) there are populations
of all ages, predominating the intermediate-age and old stars (∼2-13 Gyr). The second local
maximum corresponds to the RC and the red part of the subgiant branch and is composed
by stars with age &1 Gyr as seen in panel (c) in Figure 9. Going back to panel (b), the
CF in black corresponds to a galaxy with a constant SFR(t) (i.e., the CF of the CMD in
the panel (a)). The blue CF is from a synthetic CMD computed assuming a SFR(t) that
increased from 3 Gyr ago to the present. This CF presents a higher blue elevation due to
the bigger number of young blue stars; also the central peak is somewhat blueshifted. The
green CF represents a stellar population in which the SFR(t) dropped by 50% between 3
and 8 Gyr ago. This is reflected in the shape of the absolute maximum, where a depression
appears as a result of the assumed SFH. This kind of feature would be difficult to detect
in a real population. Finally, the red CF corresponds to a SFR(t) with a totally quiescent
period between 3 and 8 Gyr ago. The deep hollow shown in the absolute maximum of this
CF is due to the gap at intermediate ages in the SFH. The last two CFs show a higher blue
elevation as compared to a CF of a CMD with constant SFR(t) due to the higher fraction
of young stars over the whole population.
Prior to present a discussion based on CFs, we will briefly talk about the crowding effects
and, in general, the observational errors that are present in our photometry. A careful study
of the extent and nature of these crowding effects is key to study the stellar populations
present in the SMC. We will understand and quantify the crowding effects using the artificial-
star tests procedure. These artificial-star tests have been performed in a way similar to that
described in Gallart et al. (1999) and will be presented in detail in a forthcoming paper
(Noël et al. in preparation). In short, a number of artificial stars of known magnitudes and
colors are injected in the original frames, using the ADDSTAR algorithm of DAOPHOT II
(Stetson 1993). The photometry is re-done following the same procedure used to obtain the
photometry for the original frames. This process is repeated several times in order to test a
large number of artificial stars (60,000 in the case of each of our SMC fields). The injected
– 26 –
and recovered magnitudes of the artificial stars, together with the information from those
that were lost, provide the necessary information about all the observational effects present
in the photometry.
We will discuss here how the observational errors affect the CF of a few representative
fields. Those located closer to the SMC center (e.g. smc0057 and qj0111) are more affected
by crowding than the rest of the fields. To quantify these observational errors we have
simulated them for different SMC fields in the synthetic CMD of Figure 9. Following Gallart
et al. (1999), we will call the latter “model CMDs”. The model CFs (corresponding to the
model CMDs) corresponding to fields smc0057, qj0111, and smc0049 are shown in Figure 10,
together with the original CF (the CF obtained from the synthetic CMD). The observational
errors may produce significant variations in the appearance of the CF of our more central,
crowded field smc0057. Simulating the observational errors of this field in the synthetic
CMD, we obtain a model CF (dotted line) which differs substantially from the CF of the
original synthetic CMD: the absolute maximum in its CF is smaller than in the CF of the
synthetic CMD, and the blue elevation is bigger because faint stars on the low MS are
lost much more frequently than the brighter blue stars that constitute the young MS. The
dispersion introduced in the CMD when the observational errors are simulated produces an
absolute maximum that is slightly wider as shown in the dotted line in Figure 10. This
shows how crowding could simulate a non-constant SFH, mimicking a recent enhancement
of the star formation, similar to the one shown in blue in panel (b) of Figure 9. Although
still present, the effects of crowding are less severe in the case of field qj0111 since the CF of
the corresponding model CMD (dashed line) resembles quite closely the CF for the synthetic
CMD. In this field, confusion is mainly affecting the yellow stars so the main maximum is
shorter than in the synthetic CF. In the case of smc0049, it can be seen that the CF of
the model CMD (dot-long dashed line) is similar to the one of the synthetic CMD (solid
line), indicating that crowding is affecting very little the CMDs of this part of the galaxy (at
∼2.9◦). In conclusion, only the CF of field smc0057 is substantially affected by observational
errors. The effects of crowding on field qj0111 can be considered as an upper limit for fields
qj0112 and qj0116. For fields smc0100, qj0047, qj0102, smc0053, qj0037, qj0036, and qj0033
the crowding level is similar to that of smc0049. Therefore, we can safely discuss the stellar
content of all of our fields (except smc0057) by comparing their CFs straight with that of
synthetic CMDs.
Let’s concentrate now on the observed CFs of each of our fields. In Figures 11 to 13
the CF corresponding to the synthetic CMD (dashed lines) from panel (a) in Figure 9 and
the CFs (solid lines) from the observed CMDs were overlapped. Note that the shape of
the synthetic CF depends on the selection of metallicities and stellar evolution libraries.
However, small changes in the metallicity law, which result in synthetic CMDs with a color
– 27 –
0 1 2
(B-R)
Fig. 10.— Color functions of a synthetic CMD integrated over the magnitude range -
16MR63.5 assuming different levels of crowding in the data. The solid line represents the
CF of the original synthetic CMD, the dotted line corresponds to the CF of the synthetic
CMD, in which the observational errors of field smc0057 have been simulated, the dashed
line is the CF of the synthetic CMD with the simulation of errors from field qj0111, and
dot-long dashed line is the CF of the synthetic CMD with errors in field smc0049 simulated.
– 28 –
Fig. 11.— CF for the observed CMDs corresponding to the Eastern SMC fields (solid lines),
overlapped with the synthetic CF (dashed lines) from panel (a) in Figure 9, normalized to
the number of stars in the region between -0.5<(B-R)<1.5 and -1<MR<3.5. In the first
panel, corresponding to field qj0111, the CFs of synthetic populations with burst of star
formation of 30% and 50% from 1 Gyr ago to now (dotted and long-dashed line respectively)
and of 50% from 2 Gyr ago to now (dot-long dashed line) were also overplotted, showing
that there was a recent enhancement of the star formation around 1 Gyr ago in this field.
– 29 –
qj0037
(B-R
)
qj0036
(B-R
)
 (B-R
)
qj0033
Fig. 12.— CF for the observed CMDs corresponding to the Western SMC fields (solid lines),
overlapped with the synthetic CF (dashed lines) from panel (a) in Figure 9, normalized to
the number of stars in this region between -0.5<(B-R)<1.5 and -1<MR<3.5.
– 30 –
smc0057  
 
 smc0100             
 
 qj0047
(B-R
)
smc0049
(B-R
)
qj0102
(B-R
)
smc0053
Fig. 13.— CF for the observed CMDs corresponding to the Southern SMC fields (solid lines),
overlapped with the synthetic CF (dashed lines) from panel (a) in Figure 9, normalized to the
number of stars in this region between -0.5<(B-R)<1.5 and -1<MR<3.5. In field smc0057,
was also superposed the CF of a model CMD (dotted lines) in which observational errors
from this field were simulated (same as in Figure 10).
– 31 –
distribution compatible with the data have also very similar CFs. Comparison between the
observed and synthetic CFs computed assuming constant SFR(t) lets us to qualitatively
analyze the SFH of each field.
Figure 11 shows the CFs of the Eastern SMC fields. In the first panel, corresponding
to field qj0111, synthetic CFs of synthetic populations with bursts of 50% 1 Gyr ago (long
dashed line), of 30% 1 Gyr ago (dotted line), and of 50% 2 Gyr ago (dot-long dashed line)
were also overplotted. The CF of field qj0111 shows some differences with respect to the
CF of a population with constant SFR(t). In particular, the observed CF has higher values
than the synthetic one in the blue elevation (-0.3.(B-R).0.2; age.1.1 Gyr) which indicates
a SFH with enhanced star formation at young ages. This fact is also shown by comparing
with the CF of synthetic populations with bursts. In fact, the blue maximum and the main
peak of the CF with a burst of 30% 1 Gyr ago and the ones of the observed CF match very
well, pointing out that there was an episode around 1 Gyr ago of enhanced star formation in
this field which may have continued to the present time. Though a comprehensive analysis of
the CMDs will be presented in a forthcoming paper, this superposition allows us to say that
the observed CF is compatible with a SFH with an increase in the star formation of ∼30%
in the last 1 Gyr. Also note that crowding effects are not very significative in this field, as
seen from the artificial star tests. The CF of field qj0112 is a remarkable case where the
CF corresponds almost exactly with that of a population with constant SFR(t) (at least in
average). The CF of qj0116 presents a somewhat greater values of the CF in 0.(B-R).0.3
as compared with the CF of a CMD with constant SFR(t), which may correspond to stars
formed between ∼1-2 Gyr ago, possibly indicating some enhancement in the SFR(t) at those
ages in comparison with more recent ages. Note that these three fields have a very similar
CMD, and that simple comparison with isochrones gives the same information for all three:
presence of stars of all ages. The differences in their CFs are a good illustration of the
complementary information that the CF can provide. The presence in the observed CFs of
all the features that characterize the synthetic CF is the counterpart, in this representation
of the data, of the fact that the CMDs are well populated over all age ranges. The additional
information brought forward by the CFs is the relative weight of the different age ranges in
the population.
In Figure 12, the CFs of the Western SMC fields are shown. The almost complete
absence of the blue elevation in the color interval -0.3.(B-R).0.2, reflects the fact that
there are few stars younger than ∼1 Gyr. This is another example of the usefulness of the
CFs: while in fields qj0036 and qj0037 there are stars until around the 0.1 Gyr isochrone,
the CFs indicate that the relative amount of stars between 0 Gyr and 2 Gyr is substantially
less than in the case of a field with constant SFR(t). The central maximum is slightly
shifted to the red, possibly indicating that the SFR(t) started to decline around 3 Gyr ago.
– 32 –
Note that this shift is unlikely due to an overall shift of the observed CMD with respect
to the synthetic one, since the shift does not affect the red relative maximum of the CF.
In fact, this maximum is slightly shifted to the blue and higher in the CF of the observed
CMD as compared with that of the synthetic one. This is possibly due to field stars, which
contribute more in relative numbers to the poorly populated CMDs. Actually, the observed
red maximum is higher with respect to the theoretical one in the less populated qj0033. The
composition of the population in these three Western CMDs seems to be very similar, even
in the outermost field, qj0033.
Finally, Figure 13 shows the CFs of the Southern SMC fields. In the case of field
smc0057, the relative amount of young stars might be overestimated due to crowding effects
if these were not taken into account. The overplot of the observed CF (solid line) with the
synthetic (dashed line) and the model (i.e. after taking into account crowding effects, dotted
line) ones shown in Figure 13 indicate that part of the enhancement of the blue elevation
in field smc0057 is produced by observational errors but that there is still a true recent
enhancement (06t63 Gyr) in the star formation. The CF of field smc0100 is still almost
compatible with a constant SFR(t) on average, with possibly a truncation of the SFR(t) at
recent ages, as also hinted by the comparison of its CMD with isochrones in Figure 8. Moving
further away from the SMC center, the elevations corresponding to the first structure in the
CFs are less conspicuous, indicating that young stars are less common and intermediate-
age stars dominate the fields. The fact that the main peak is redder from field qj0047 on
(except, maybe, in the case of field qj0102 which is situated more towards the East than
the other Southern fields), points out that there is a larger amount of old stars and, like in
the Western fields, that possibly the SFR(t) started to decline around 3 Gyr ago. As in the
case of the Western field qj0033, the second, red relative maximum in the CFs gets bigger
with increasing galactocentric distance. The reasons for this are twofold. First, the amount
of stars in the RC and in the RGB, relative to the total stellar content is larger at larger
distances from the center (even though not large differences among fields seem to be present
beyong r≈2.7◦), where the age of the stellar population is older on average. Second, the
contamination by foreground stars is larger relative to the total number of stars from the
galaxy. This last factor, may be the main player in the case of field smc0053.
5. SUMMARY
We obtained B and R-band photometry of stars from 12 SMC fields observed during
4 different campaigns with the C100 telescope at Las Campanas Observatory. The spatial
distribution of the fields samples different parts of the galaxy, both in areas with large
– 33 –
amounts of recent star formation such as the “Wing” area and “undisturbed” regions at the
West and towards the South part of the galaxy, in which the stellar populations may be
representative of the underlying population of the SMC formed prior to the events of star
formation that shaped its current irregular morphology. The stellar content present in these
SMC fields has been analyzed by means of a set of [B-R, R] CMDs that reach the oldest MS
turnoffs (MR∼3.5) with an excellent photometric accuracy.
In this first aproach to study the SFH of our SMC fields, we found the following. The
fields in the “Wing” area contain very young blue stars and show a broad MS turnoff/subgiant
region and a wide range in luminosity of the RC, pointing out that star formation in these
parts has extended from at least ∼13 Gyr ago to the present with no substantial gaps, as the
areas around all the overlapped isochrones are well populated. Field qj0111 (the closest to
the center of the SMC in this “Wing” area) seems to have experienced an enhancement in its
recent star formation, compatible with an enhancement of 30% in the SFR(t) over the last 1
Gyr. This is indicated by the height of the blue elevation its CF (color interval in the range
-0.3.(B-R).0.2) as compared with that of CFs corresponding to synthetic populations with
different SFR(t). The other two fields analyzed in this direction seem to have had a SFR(t)
close to constant on average.
Very little star formation has been going on from ∼1 Gyr ago until now in the Western
fields, as indicated by the much lower amount of young blue stars and the lack of the blue
elevation in the CFs. Considering the RC (formed by stars older than ∼1 Gyr) of fields
qj0036 and qj0111, both located at the same galactocentric distance, we found that the
number of stars is comparable, indicating that the integrated SFR(t) from old ages and until
∼1 Gyr ago in both fields is similar, and that there was a mechanism in the “Wing” area
that triggered the star formation around 1 Gyr ago, in particular, in the location of field
qj0111. Field qj0033, though located further away from the center in the Northwest, presents
a distribution of stellar ages similar to that of the two other Western fields, as seen from the
resemblance of the three CFs and from its CMD, in which the area below the turnoff of the 4
Gyr isochrone is still quite populated. In fact, the apparent differences between the CMD of
field qj0033 and the other two are due to the much larger number of stars populating those.
If only a subset of stars of those CMDs are represented, to equal number of stars in the
CMD of qj0033, the distribution of stars around the different isochrones is very similar. In
these three fields, the bulk of stars seems to be older than 3-4 Gyr. A similar conclusion was
reached by Dolphin et al. (2001) for a field located in the Northwestern part and relatively
close to field qj0033 (see Figure 1), where they found a greatly decreased star formation in
the past 2 Gyr.
Regarding the fields observed toward the South, the young population is less important
– 34 –
from r=2.7◦ on. The blue elevation in the CFs of the Southern fields is only found in the
two fields closer to the center. In the case of smc0057, its shape is consistent with some
enhancement of the recent SFH as compared to a constant SFR(t). From the CFs it is
evident that field smc0100 has many more stars younger than 2 Gyr (relative to the total
population of the field) than the Western fields qj0036 and qj0037, even when it is almost 1◦
further from the SMC center than the latters. Note that this field is located at the border
of a more densely populated isopleth than qj0036 and qj0037 and in the part in which the
trumpet-like distribution of the young population fans out. Beyond ∼2.7◦, there are only
few stars younger than 3 Gyr old and the differences between the fields are small (except for
the fact that the density of stars in field smc0049 is larger than in the other two). Finally,
except for Eastermost field qj0102, the further South from the SMC center we go, the more
is the main peak of the CF shifted to the red. This, together with the above facts, may
indicate that the main epoch of star formation beyond ∼2.2◦ in this direction ended around
3-4 Gyr ago.
6. CONCLUSIONS
The SMC shows a clear morphologic dichotomy between its young and old population.
The youngest component has an asymmetric distribution which fans out towards the “Wing”
area in the Northeast, similarly to the HI distribution (Stanimirović et al. 1999), while the
RGB and AGB stars have a more symmetric, spheroidal distribution. Using deep (down to
MR = 5.5) CMDs in 12 small fields that strategically sample different SMC regions, we are
trying to shed some new light into our knowledge of the SMC evolution, and answer some
of the questions posed in the Introduction.
We found that the underlying spheroidally distributed population is mainly composed
by intermediate-age and old stars, and its distribution does not show strong galactocentric
gradients. Our fields situated toward the Northwest of the bar, at galactocentric distances
from 1.3◦ to 2.9◦ contain very few stars younger than ≃ 3 Gyr. The comparison of their CFs
with that of a synthetic population with constant SFR(t) indicates there has been an actual
drop of the SFR(t) at around this age until the present. Even though, some residual star
formation seems to have continued up to now. No strong differences can be noticed between
the CMDs and CFs of the fields at 1.3◦ and 1.4◦ and the one at 2.9◦. The apparent differences
between these CMDs are mainly due to the different number of stars in them, rather to a
fundamentally different composition of the stellar populations. Something similar occurs in
the case of the Southern fields beyond ≃ 2.2◦. In addition, we estimated that the SFR(t)
at intermediate to old ages in fields located at the same distance from the SMC center and
– 35 –
at either side (e.g. qj0111 and qj0036) is similar. With the current analysis of the data we
cannot provide a detailed SFH for these fields, and therefore we cannot confirm nor rule out
periods of quiescence as found in other studies that used shallower data. This will be the
subject of a forthcoming paper.
The three fields situated towards the East, in the “Wing” region, show very active
current star formation. In the case of the field closer to the center, qj0111, we estimated
that the current star formation rate (from around 1 Gyr ago to the present) in this field
is ∼30% larger than the SFR(t) averaged over the galaxy’s life. However, the other two
northeastern fields, situated just slightly further away from the center, have a CF which is
compatible with that of a constant SFR(t) over the whole galaxy’s history. Therefore, only
the parts of the Wing closer to the center, seem to be undergoing an exceptionally intense
episode of star formation at the present time.
At the radius of the innermost field (∼1 kpc), we derived a crossing time of ∼108 yr,
obtained adopting a measured velocity dispersion of 36 km/s (Carrera 2006, using the stars
below the RGB tip corresponding to our SMC fields). In the case of our outermost field (∼4
kpc) the crossing time is ∼2×108 yr. Large scale asymmetries should disappear within a
few crossing times, and the population older than ∼1 Gyr is then expected to be well mixed
at a radius of ∼1 kpc, while the population older than ∼2 Gyr is well mixed at ∼4 kpc.
Hence, although our fields only cover little isolated parts of the SMC (as compared with the
huge area embraced by HZ04), they are representative of the SMC populations older than
∼2 Gyr.
The larger amount of young stars present in the Eastern fields may be related to a recent
interaction between the SMC, the LMC, and the Milky Way as is suggested by numerical
models (e.g. Yoshizawa & Noguchi 2003). Note that the presence of a considerable young
population in the eastern fields and lack thereof in the western ones is in good correspon-
dence with the existence or absence of large amounts of HI at the corresponding locations
(Stanimirović et al. 1999). It is interesting to notice that this trend is not maintained in the
closest Southern field, smc0057, in which there is a considerable amount of young population
but the amount of HI is small.
The presence of a substantial amount of intermediate-age population in our outermost
SMC fields, could be a sign that a few gigayears ago HI gas extended as far as ∼4◦ and has
since gradually receded to the more central regions. Another possible explanation for this
is that tidal interactions happened periodically, and then these stars dynamically mixed,
resulting in old stars (those from previous passages) being symmetrically distributed and
the younger ones only in the current tidal feature. None of the studied fields is dominated
by an old stellar component, as one would expect for an old stellar halo similar to the one
– 36 –
of the Milky Way. This may mean that a disk population is still dominating over a possible
old halo, if it does exist in the SMC.
We want to thank Antonio Aparicio and Santi Cassisi for many very useful opinions
and discussions and a careful reading of the manuscript. We are very grateful to the anony-
mous referee for a critical and useful report that helped to improve the paper. The authors
acknowledge support by the Plan Nacional de Investigación Cient́ıfica, Desarrollo, e Inves-
tigación Tecnológica, (AYA2004-06343). E. C. and R. A. M. acknowledge support by the
Fondo Nacional de Investigación Cient́ıfica y Tecnológica (No. 1050718, Fondecyt) and by
the Chilean Centro de Astrof́ısica FONDAP (No. 15010003). This project has made generous
use of the 10% Chilean time, and continuous support from the CNTAC and Las Campanas
staff is greatly appreciated.
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This preprint was prepared with the AAS LATEX macros v5.0.
	INTRODUCTION
	OBSERVATIONS AND DATA REDUCTION
	THE PHOTOMETRY
	Photometry of SMC fields
	Standard Stars Photometry
	THE SMC STELLAR CONTENT
	Theoretical isochrones
	Color Functions
	SUMMARY
	CONCLUSIONS
