Issue |
A&A
Volume 503, Number 1, August III 2009
|
|
---|---|---|
Page(s) | 87 - 101 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/200912045 | |
Published online | 22 June 2009 |
The star cluster population of the spiral galaxy NGC 3370![[*]](/icons/foot_motif.png)
M. Cantiello1 - E. Brocato1 - J. P. Blakeslee2
1 - INAF-Osservatorio Astronomico di Teramo, via M. Maggini
snc, 64100 Teramo, Italy
2 -
Herzberg Institute of Astrophysics, National Research Council of
Canada, 5071 W. Saanich Rd, Victoria, BC V9E 2E7, Canada
Received 12 March 2009 / Accepted 10 June 2009
Abstract
Aims. We study the photometric and structural properties of the star cluster system in the late type Sc spiral NGC 3370.
Methods. BVI observations from the Advanced Camera for Surveys on board of HST are used to analyse in detail the colours, magnitudes and spatial properties of cluster candidates. The final catalogue of sources used for the study is composed by 277 objects.
Results. The colour distributions of cluster candidates appear multi-modal. Although firm age constraints need the use of more age-sensitive indicators, the comparison of cluster candidate colours with the colours of Galactic and Magellanic Clouds star clusters, suggests an age difference between the various sub-peaks, with a red old sub-system, a rich population of intermediate age (1 Gyr), and a blue tail of very young (below
100 Myr) clusters. The luminosity functions appear normal for this type of galaxy, as for the distribution of cluster effective radii (
). Our analysis suggests the presence of a peak in the
distribution at
3.0 pc, with blue (likely young) cluster candidates showing smaller radii respect to red (likely old) objects. Finally, inspecting the properties of candidate globular clusters, we find a colour distribution matching with Galactic Globulars, with a median [Fe/H]
dex, though a non negligible tail towards lower metallicities is also present.
Key words: galaxies: individual: NGC 3370 - galaxies: star clusters
1 Introduction
The study of star clusters in galaxies provides an accurate and relatively straightforward tool to unveil the mechanisms that produced the present organisation and evolutionary properties of stars in the galaxy. Star clusters allow to inspect the host galaxy both as a system and as single star clumps hosting - relatively - simple stellar populations. Moreover, stellar clusters are the cradle of a large fraction of stars (e.g. Lada & Lada 2003, and references therein). As a consequence, understanding the properties of the Star Cluster (SC hereafter) system in a galaxy helps understanding the properties of the host galaxy. Furthermore, SCs are relatively simple stellar systems - in first approximation single age and single metallicity stellar populations - much simpler than the stellar system of the host galaxies, providing the natural bridge from local single star analysis to distant unresolved stellar population studies.
Motivated by the chance to analyse the evolutionary properties of the host galaxy, in the last decade, especially after the HST refurbishment, a great deal of work has been dedicated to the study the properties (luminosity, radius, mass, etc.) of the SC system in spiral and irregular galaxies (e.g. Larsen & Richtler 2000; Whitmore & Schweizer 1995; Whitmore et al. 1999; Gieles et al. 2006a; Bik et al. 2003; de Grijs et al. 2003; Gieles et al. 2006b, just to quote few examples).
In this work we present a study of the SC system in the spiral galaxy NGC 3370, based on archival multi-band images taken with the HST Advanced Camera for Surveys.
The galaxy is a nearly face on Sc spiral (Hubble type SA(s)c, de Vaucouleurs et al. 1991), showing an intricate tangle of arms, and mass similar to our own Milky Way. NGC 3370 was the host of the type Ia Supernova SN 1994ae (van Dyk et al. 1994). The light-curve of this SN Ia is one of the nine templates used by Riess et al. (1996) to introduce the SNe Ia multicolour light-curve shapes method to estimate distances. With the advent of the high efficiency ACS camera on board of HST, and thanks to the specific properties of the galaxy (face on, relatively nearby spiral), NGC 3370 has been targeted by an HST program to study the light-curves of Cepheids, to provide a direct calibration of the SN Ia distance (Riess et al. 2005). The program, carried out on optical Vand I images, has been integrated by complementary B band exposures for the Hubble Heritage program.
The optical BVI data available offer an excellent opportunity to investigate accurately not only the photometric, but also the structural properties of the SC systems in this spiral, thanks to the high resolution and small PSF FWHM of the ACS.
The paper is organised as follows. In Sect. 2 we present the observational dataset used, the data analysis carried out, and the detection and selection criteria chosen for SC candidates. The study of photometric and spatial properties and the comparison with models is discussed in Sect. 3. We present our conclusions in Sect. 4.
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Figure 1:
ACS B, V and I composite image of NGC 3370, the image size is
roughly
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Table 1: NGC 3370 properties and observations.
2 Observations, data analysis and star cluster selections
The ACS/WFC camera observations of NGC 3370 used in this work come
from two different proposals. The proposal ID #9351 (P.I. A. Riess)
consists of very deep F555W (V) and F814W band (
I)
observations to study the Period-Luminosity relation of the Cepheids
in the galaxy (Riess et al. 2005), with the purpose of deriving the
distance of NGC 3370 and provide a precise luminosity calibration of
the Type Ia supernova observed in the galaxy. The study realised by
Riess et al. provided the farthest direct measurement of
Cepheids. The other set of F435W band (
B) images was
obtained for the Hubble Heritage (proposal ID #9696, P.I. K. Noll). A
colour image of the galaxy is shown in Fig. 1. The main
properties of NGC 3370, and of the observational dataset used are
reviewed in Table 1. For the distance modulus, we adopt
Riess et al. value,
,
derived from an
empirical calibration of Cepheids' Period-Luminosity relation, and an
LMC distance modulus of 18.50 mag.
Standard reduction was carried out on raw images using the APSIS image
processing software (Blakeslee et al. 2003). Since ACS/WFC images are
under-sampled for wavelengths at
Å, and
thanks to the fine dithering of the input images, a resolution better
than the ACS detector pixels size, 0.05
/pixel, can be achieved
with these images. We adopted a resampling of 0.035
/pixel as
input parameter for APSIS, which corresponds to
5 pc/pixel
at the galaxy distance.
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Figure 2:
Upper to lower panel: radial I, V and B band surface
brightness profiles of NGC 3370. The linear fit to the data at
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After cosmic-ray rejection, alignment, drizzling, and final image
combination, we derived the sky background from the median counts in
the image corner with the lowest number of counts. This assumption is
supported by the fact that the surface brightness profile of the
galaxy is practically constant for
(Fig. 2).
The source detection was obtained using SExtractor (Bertin & Arnouts 1996)
independently on the V and I frames. Due to the low S/N of B-band
images, the source detection in this band was done using SExtractor in
the pixel association mode (ASSOC mode), adopting as reference
the coordinates of sources detected in the I-band frame. We used a
minimum of 5 connected pixels and 2
threshold for sources
detection. This resulted in a list of
20 000 objects. The
coordinates of sources detected from V and I frames were
cross-checked, allowing a maximum wandering of 4 pixels
, then we
performed a first very bland selection of SC candidates based on the
SExtractor parameters star/galaxy classification, object
major-to-minor axis ratio, and FWHM (object with CLASS_STAR = 0.00,
elongation A_IMAGE/B_IMAGE
2.5 and
were rejected).
Moreover, we rejected the sources fainter than mI=27.5, and
mV=28.5 mag
. Using such limits we ended up with a list of
8000 SC candidates whose structural properties were then
analysed.
Given the linear pixel scale of these NGC 3370 images, and the ACS
Point Spread Function FWHM of 2.5 pixels, we are in the
condition of using the ishape software (Larsen 1999) to
estimate the spatial extension of SC candidates. This software package
allows to determine the physical characteristics of SC candidates
(
,
elongation, etc.) by convolving analytic profiles with the
PSF, then best-fit parameters are obtained by the
minimisation. Ishape provides accurate intrinsic FWHM values of
slightly resolved objects down to 1/10 the FWHM of the PSF,
corresponding to
1.2 pc in our case. In other words, provided
that a good PSF sampling can be obtained, effective radii of star
clusters
1.2 pc can be retrieved. The input PSF to be
used for ishape needs to be subsampled by a factor 10 with
respect to the input science images. As suggested by the ishape handbook,
we generated our PSF using the SEEPSF task of DAOPHOT within
IRAF
. To avoid contamination from clusters,
the list of stars to determine the PSF was selected on the basis of
the FWHM, colours and magnitudes from DAOPHOT. We finally used 10
bright stars (all common to the catalogue of comparison stars in Table
3 of Riess et al.), evenly distributed on NGC 3370, and all at
distances >
from the centre of the galaxy. It is useful to
anticipate here that a posteriori all the objects used as
template for the PSF, and all the Cepheids detected by
Riess et al. were catalogued as stars by ishape .
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Figure 3:
Central panel: effective radii from the I-band frame versus
the V-band
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Among the various profiles available with ishape, we choose a
Moffat profile with a power law index -2.5, since it gave generally
better residuals compared to other choices. A Moffat profile has
already been shown to be effective in fitting the profiles of both
young and old star clusters, though with slightly smaller exponents
with respect to our choice (see,
e.g., Larsen 1999; Mackey & Gilmore 2003; Elson et al. 1987). As discussed in Larsen (1999),
the details of the model profile chosen are not an issue as long as
the the
values are derived for sources with intrinsic sizes
smaller or similar to that of the PSF, as in the present case. The
analysis was carried out independently on the I, V, and B frames,
although only I and V band data were finally used to estimate the
average effective radii of SC candidates.
The ishape output parameters were used to further constrain the list of SC candidates. In particular, we reject the objects:
- whose effective radii
differ more than 2
in the two bands (Fig. 3). The
are derived using standard error propagation on ishape fitted parameters and uncertainties. In few cases the output of the fit is very good in both bands, so that the rms is small for V and I
, and the object will end up rejected by a simple 2
rejection criterion. However, if the systematic uncertainties arising, for example, from the PSF, the analytic profile chosen, etc., are taken into account, then the two sources should be included in the catalogue. After several tests, we decided to use a default systematic uncertainty of
15%
. Then, for the 2
selection we used the maximum
between the rms from ishape , and
15%
;
- with
(Larsen 1999);
- with too small/large
. The specific properties of Moffat profile chosen allow to estimate effective SC radii below the
1.2 pc limit aforementioned (see Larsen 1999, and ishape user's guide). However, we choose to adopt as lower and upper rejection limits
< 1.5 pc, and
> 20 pc, respectively. As a reference, using the data from McLaughlin & van der Marel (2005),
1
of massive star clusters in the Milky Way and its satellites have
< 1.5 pc, while
3
have
> 20 pc;
- elongation (major to minor axis ratio) >2.0, comparable to
the maximum observed in Magellanic Clouds star clusters (van den Bergh & Morbey 1984).
Figure 4: Some examples of visual classifications codes. For each source we show the original I-band image ( upper sub-panels) and the ishape residuals ( lower sub-panels). Objects associated to the classes 33 (large residuals, crowded area), 100 (possible background galaxies), and stars are rejected in the final catalogue of SC candidates.
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To verify the goodness of the ishape best fit parameters we have visually inspected all sources, introducing a sub-classification of sources depending on the residuals of SC candidates subtraction, and on the crowding. The visual classification code was used for further selections. Figure 4 shows some examples of sources with different visual classification. The visual class code that we used is a number composed by two digits, the first associated to the goodness of ishape residuals, the second to the level of crowding. For both digits the range adopted is 1-3. For the first digit 1/2/3 means good/satisfactory/large residuals, respectively. The second is related to crowding with 1/2/3 meaning no crowding/less/more than three sources within 20 pixels from the SC candidate. As an example visual class=12(31) means good residuals and 1 or 2 sources within 20 pixels (large residuals and no other source within 20 pixels). A default visual class=100 is adopted for diffuse objects (likely background galaxies) showing very large residuals in the ishape subtracted frame (see Fig. 4).
The aperture photometry of all the sources selected has been obtained using the Phot/Apphot task under IRAF. Due to the high, strongly variable background in some regions of the galaxy, we made different tests using 3, 5 and 7 pixels aperture radius, and 10, 16 pixel annulus for background determination. As a final choice, we adopted 3 pixels aperture for the photometry, while the background was estimated in an annulus 16 pixels inner radius and 3 pixel width.
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Figure 5: Aperture corrections in B, V, and I-band versus the SC candidate radius. The solid lines show the best fit linear equation. |
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Table 2: Number of objects rejected per selection criteria.
Dealing with slightly extended objects having different radii, the
aperture correction depends on the radius of the cluster. As a
consequence, we fitted the aperture correction versus
.
To avoid
contamination from galaxy background, uncertain
estimates, and
crowding, we decided to use only sources brighter than
mag, ishape S/N>50, visual class
23,
and local surface brightness background
mag
(galactocentric radius
). Aperture magnitude was
derived in 3 and 6 pixels (
15 and 30 pc) apertures over the
selected sources. Figure 5 shows the aperture correction
derived as the difference between 3 and 6 pixels aperture magnitudes,
versus the effective radii. The best fit linear correlations shown in
the figure for each passband was then used to correct the magnitudes
of all SC candidates in B-, V-, and I-band.
The correction from 6 pixels to ``infinite'' radius, as well as the transformations from the F435W/F555W/F814W ACS filter system to standard B/V/I filters, and foreground extinction, were applied following the prescriptions by Sirianni et al. (2005).
Once all corrections were made, we added new constraints to further
clean the final list of SC candidates. In particular, to eliminate
objects with very high internal extinction and possible distant
background galaxies, we considered only those sources with
mag,
mag (typical maximum colours for globular
clusters), and a maximum photometric uncertainty
mag. SC candidates showing large residuals and in crowded
regions, candidate background galaxies (visual class =33 and 100,
respectively) as well as sources located in regions with strongly
variable background (to avoid objects with photometry significantly
contaminated by internal extinction) have been rejected, too. The
final list of SC candidates matching with the required constraints is
composed by 277 objects
. A schematic view on
the effects of the various selection criteria applied, with more
details on the numbers, is reported in Table 2. The
table gives the number of objects before (
)
and after
(
)
each selection criteria is applied, together with the list
of criteria adopted and the number of candidates rejected with the
chosen parameter (
). It is worth noting that the same object
might satisfy two or more rejections, thus the total number of objects
rejected,
,
is not simply obtained by summing up the
numbers in the
lines. The positional, photometric and
structural properties of the final catalogue of sources are reported
in Table 3.
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Figure 6:
Colour-colour diagram of the SC candidates. Dark-grey dots,
empty and full circles mark the positions of the sample after the
first, second and third (final catalogue) selections described in
Table 2. The grey shaded area marks the region of
SPoT-SSP models by Raimondo et al. (2005). The arrow shows the direction of the reddening
vector. Five pointed stars are ``outlier'' SC candidates, possibly
associated to intermediate age clusters. The insert
panel shows the SC candidates (full dots), the SC outliers
(five-pointed stars), and the standard SPoT SSP models (grey-shaded
area). The dark-grey area shows the region occupied by SSP realisations
of the recent SPoT models by Raimondo (2009), computed paying
particular attention to the stochastic effects of TP-AGB stars. Only
ages between 0.3-2 Gyr and [Fe/H] |
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Figure 7: Left panels: B-V colour magnitude diagram ( upper panel) and colour histograms ( lower panel) of SC candidates. Right panels: as left, but for B-I. The arrows indicate the median colour of GGCs. |
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3 Discussion
3.1 Analysis of colours
Table 3: Structural and photometric properties of selected SC candidates. The full table is only available in electronic form at the CDS.
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Figure 8:
Colour histograms of the comparison galaxies (as labelled in
left panels). Dotted lines show NGC 3370 SC candidates. For NGC 3367
and SMC a different binwidth is used, because of the smaller number of
SCs (see
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Figure 6 shows the colour-colour diagram of the final
catalogue of SC candidates. In the figure it is shown also the effect
of the various steps of the selection. Dark-grey dots, empty and
filled circles mark the position of the sample after the selections
based on SExtractor, ishape , and photometric parameters,
respectively. The full circles in the figure refer to the final
selected sample of SC candidates. Also shown in the figure, with a
grey area, is the region of the SPoT Simple Stellar Populations models
for metallicity between [Fe/H]
dex, and ages in the
interval 25 Myr
14 Gyr (see Raimondo et al. 2005, for more details on SPoT SSP
models). As expected, the data overlap to SSP models,
since SC are, at least in first approximation, well represented by
SSPs. It must be emphasised, however, that such overlap is not a
trivial result. In fact, in the selections described in the previous
section, the only constraint on colour was on the maximum V-I and
B-V allowed.
One interesting feature appearing in Fig. 6 is the
non-negligible number of objects located at
and
(five pointed stars in the figure). After different
counter-checks, we concluded that there is no obvious reason to reject
these clusters from the final catalogue. As shown by the arrow in the
panels, even an internal extinction
mag would not
shift these SC candidates in the region of SSP models. Moreover, such
high extinction is unlikely since such objects do not appear obviously
associated to regions of high internal extinction, while they are
rather evenly distributed over the area of the galaxy. One possible
interpretation of these objects is that they are intermediate age
SCs (
(Gyr)
2). Within this age interval, the
emission of Thermally Pulsating AGB stars (TP-AGBs) dominates the
light emitted by the SC, in particular in the long-wavelength regime
(
8000 Å; see, e.g. Maraston 2005, and references
therein). However, the presence of stars in such
evolutionary stage is strongly influenced by stochastic effects. As a
consequence, the stochasticity due to the number of cool TP-AGBs can
significantly affect the integrated colours of the stellar system. To
highlight such behaviour, the insert panel in Fig. 6 shows
the sample of selected SC candidates, and the ``outliers'' at
and
mag (five-pointed stars), together with
the region where the recent SSP models by Raimondo (2009) for
intermediate ages and [Fe/H]
dex are distributed (dark-grey
area). The new set of models used has been computed with an updated
version of the SPoT code, paying particular attention to the
statistical effects generated by Thermally Pulsating AGBs. In the
figure, the dark-grey area shows the distribution of models when the
stochastic effects due to TP-AGB stars are properly taken into
account. As shown in the insert, these models predict the existence of
the outliers (optical models have been provided as a private
communication by Raimondo, for more details on models and near-IR
colours see Raimondo 2009). In a following section we will discuss
more in details the data to models comparison for the whole
sample of SC candidates.
Figure 7 shows the colour magnitude diagrams and colour histograms for the SC candidates. It is not surprising that the whole population of SC candidates in NGC 3370 does not have a unimodal colour distribution, showing the presence of sub-peaks possibly associated to different SC sub-populations.
As a matter of fact, since NGC 3370 is a late type Sc spiral, it is
expected that this class of galaxies is actively forming stars, and
star clusters. Thus, populations of young/intermediate age SC are
expected to host in the galaxy, in addition to the old population of
Globular Clusters (GCs). To highlight this point, in the colour
histograms shown in Fig. 7, we have added an arrow
showing the median colours of Galactic GCs (GGCs,
,
mag for
90 GGCs
with
mag, data from Harris 1996). It is rather
obvious, then, to conclude that the red peak observed in the lower
panels is actually due to the GC population in the galaxy.
If the intermediate peak and the blue tail of SC candidates are taken
into account, still using as reference the system of young open
clusters (OCs) in the Galaxy, we find that the OCs at
,
and
mag have ages
(based on only 3 Galactic OCs), while blue OCs at
,
and
mag have on average
(based on 11 OCs)
.
Given the results of such comparison with Galactic star clusters, it
is reasonable to conclude that the colour peaks observed in Fig. 7 are mainly driven by age differences between the blue/intermediate/red SC candidates.
The situation, however, might be complicated by the possible presence
of residual internal extinction. Since the galaxy is oriented nearly
face on, the effect of internal extinction is minimised. Moreover, as
discussed in previous section, to reduce possible extinction present
in the dusty, star forming regions we rejected the sources located in
areas of strongly varying background, or where dusty patches can be
recognised. The presence of the colour peaks discussed above is an
additional indirect probe against a possible strong contribute of
internal reddening: a significant amount of dust extinction, in fact,
should smear out such features. However, it is not possible to exclude
at all the presence of some residual internal extinction. To have
other indications about the possible nature of the colour range and
sub-peaks in NGC 3370, we compare the B-I and B-V colour
histograms of SC candidates with the same data for other galaxies,
some of which are corrected for internal reddening. In particular, we
use the data from 1) Milky Way's GCs (Harris 1996), and Open
Clusters (Lata et al. 2002); 2) NGC 3367 from García-Barreto et al. (2007); 3)the data of 20 Spirals from Larsen (1999); 4) M 33 data
corrected for reddening (Park & Lee 2007); 5) SMC Star Clusters from
Rafelski & Zaritsky (2005); 6) LMC data from Bica et al. (1996). All the
data used are in (or are transformed to) the standard photometric BVIbands. The comparisons between different galaxies are shown in Figs. 8 and 9. In order to compare only SCs in the
luminosity range of the SC candidates considered here, we have
excluded all SCs having total absolute magnitude
mag.
Figure 8 shows B-I and B-V colour histograms of the SC in the MW, NGC 3367, the spirals from Larsen (1999), M 33 and the SMC. The galaxies are ordered according to their morphological T-Type, all histograms are normalised to have 1 in the most populated bin. In each panel of the figure the colour histograms of SC candidates in NGC 3370 are shown with dotted lines.
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Figure 9:
B-V colour histograms of LMC Star Clusters (solid lines)
and NGC 3370 (dotted lines). The vertical blocks refer to LMC
clusters selected according to the SWB class: the first, second and
third row refer to LMC clusters with SWB
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By inspecting the colour histograms it is easy to reveal similarities
and differences between the system of SC candidates in
NGC 3370 and in other galaxies. One example is represented
by the red sub-peak, which appears quite similar to the red sub-peak
in the colour distribution of SMC clusters. Using the age
estimates by Rafelski & Zaritsky (2005) we find that the 20 SMC clusters
with
mag have a median age
Gyr. The range of
colours generally shown by other systems is quite similar to that of
NGC 3370. The only exception is represented by the colour
histograms of the SCs from Larsen (1999). However, the selection
criteria used by Larsen exclude SCs with
,
which represents
45% of our sample of objects. In
addition, the very blue/young stellar clusters are rejected by Larsen,
adopting a lower limit to the H
colour. Thus, we are lead
to conclude that, rather than a systematic difference between our data
and Larsen's, the observed differences are due to the
intrinsically different SCs selection. In any case, the peak of the
distributions of Larsen's data appears similar to the
main peak of NGC 3370 SCs, though slightly shifted towards
bluer colours.
The SCs data of NGC 3367 - the galaxy of the sample morphologically more similar to NGC 3370 - do not show obvious multi-modal colour distributions. The range of colours, and the position of the main peak are roughly similar to NGC 3370. As for what concerns SMC clusters, the colour distributions span over the same range, and the peak of SC sub-systems seems to be recognised here as in NGC 3370.
We provide in Fig. 9 a separate comparison to LMC
data. The reason for keeping LMC data aside is that, in this case, we
can play with the age of the selected clusters by using the SWB class
(Searle et al. 1980) of LMC clusters, and also make a test on the internal
extinction in NGC 3370. The figure shows the B-V colour histograms
of LMC clusters, corrected for internal extinction, and NGC 3370 SC
candidates. Each row of panels in the figure shows NGC 3370 cluster
candidates dereddened adopting a different average internal
extinction,
and 0.2 mag
from upper to lower panel, respectively. In addition, assuming the
SWB classes from Bica et al. (1996), each column of panels is obtained
assuming a lower limit to the SWB. Specifically, the first column
includes all SWB classes, while the other two include only LMC
clusters with SWB
3 and 6, respectively (labels in the uppermost
panels). All panels show NGC 3370 colour histograms (dotted lines)
shifted according to the internal reddening assumed, and the LMC
clusters colour histograms using the SWB selection criteria (solid
lines). Some hints on age distributions and, possibly, internal
extinction of the SC candidates can be derived by a careful inspection
of this figure. The upper panels show that if old LMC clusters are
taken into account (SWB
,
yr), there is a good
match between NGC 3370 red peak and the old clusters in LMC. Thus, we
have an additional indication that this population is, in fact,
composed by old GC candidates. It is worth to notice, in the case of
and SWB
(central
panel in the figure), the similarity between the main colour peaks of
the two galaxies. Clearly, because of the differences between the two
galaxies, it is not possible to conclude whether or not such good
matching is a consequence of an average internal extinction of
0.1 mag on a SC system in NGC 3370 with an age distribution
similar to LMC. It is, however, reasonable to take this value as an
upper limit for
.
Furthermore, the
lower panels, which assume larger internal extinction, show that such
average reddening would move the main peak to a colour corresponding
to ages of the order of
- obtained taking MW OCs
and LMC clusters ages as reference. Although young SCs are expected to
be present in late type, actively star forming galaxies, it is not
reasonable to conclude such predominance of very young objects. The
position of the red peak is not an issue in the latter case, since it
is expected that old clusters are, on average, less affected by dust
extinction being far from actively star-forming regions. Thus, the
shift of the red peak for
mag
is not probable. However, since this test is carried out using a common average value for internal extinction, we cannot rule out high
extinction values on single bluer/younger cluster candidates.
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Figure 10: Upper panels: colour histograms of SC candidates, the position of the three relative peaks is emphasised in each panel with dashed lines. Lower-left panel: spatial distribution SC candidates selected according to their membership to the colour sub-peaks (see text). Five pointed stars/full squares/circles mark candidates in the blue/intermediate/red tail respectively. |
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Figure 11:
Annuli division used to compute completeness functions. The
regions are characterised by their median surface brightness:
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In conclusion, the comparison of the colour histograms for NGC 3370
SC candidates with other SCs from literature shows that the range of
colours appear normal with respect to similar class of
galaxies. Clearly, the comparisons shown cannot be used to constrain
ages, or any residual internal reddening, because of the intrinsic
differences existing between the galaxies. However, we can give some
limits, in particular, it is reasonable that NGC 3370 hosts three
sub-populations of SC candidates: one with colours typical of old GCs,
one with very blue colours, characterising a population of very young
SCs, and a rich population of intermediate age SC candidates. This
expectation is partly supported by the spatial distribution of the SC
candidates in the three colour peaks, shown in Fig. 10. In the figure we used the position of the three
relative maxims to define a preliminary centre of each sub-peak in B-Iand B-V. Then, the median and standard deviation of the sole SCs
within half-distance from the sub-peaks is obtained (dashed-lines in
the upper panels). All SC candidates within
from the median value of the peak in both colours are then
selected. The SCs selected in this way are shown in the lower-left
panel of the figure: five pointed stars/full squares/circles mark
candidates in the blue/intermediate/red tail respectively. By
inspecting the spatial distribution of clusters, we recognise that the
SC candidates in the blue tail are mostly located near the galactic
centre, while the star clusters in the other colour bins are more
spread over the galaxy, with the ones in the red peak being on average
more distant from the centre of the galaxy, as expected for GC
candidates. The median effective galactocentric distance of each SC
class is estimated and reported in the figure.
3.2 Luminosity functions
Starting from the work by Elson & Fall (1985) on LMC SCs, empirical data from a large sample of spiral and irregular galaxies have shown that the Star Cluster Luminosity Function (SCLF) usually follows a power law, with a sharp turnover at faint magnitudes. In this section we analyse the LF profile of the SC candidate system in NGC 3370.
To properly study the SCLF, we need to take into account the
completeness corrections in the different bands. However, because of
the selection criteria adopted, this is a complex task. In our case,
in fact, the completeness functions should take into account i) the
photometric completeness; ii) the selection on sizes, and iii) the
visual identification. While the first two contributions to the
completeness can be somehow obtained from numerical experiments, the
third one is less straightforward to derive, if feasible at all.
Moreover, the completeness fraction is different for objects of
different sizes. For such reasons we choose to adopt the following
approach: the galaxy is divided in four concentric regions, selected
on the basis of the median surface brightness of the galaxy. In
particular, we choose
20,
,
,
and
as
separation between the regions #1, #2, #3, and #4. Figure 11 shows the four regions and the position of SC
candidates. In each of the four annuli, then, we run completeness
tests separately. To add artificial SCs we used DAOPHOT/ADDSTAR,
adopting a template SC candidate derived from the best candidates in
our list. Accurate completeness functions would need different
numerical experiments obtained with SC templates of various
.
We
have not carried out such detailed analysis. It is worth to remark,
though, that the median size of template SC,
pc, is representative of the vast majority of the SC
candidate population (see next section).
![]() |
Figure 12: B, V and I-band completeness functions for the each of the four annuli considered (labelled in the panels). For each one of the 4 annuli, we have carried out several numerical experiments shifting the grid of artificial stars. Different experiments are shown with different line types in each panel. The horizontal dotted line marks the 90% completeness limit in the annulus. The rightmost panels show the median completeness function for each annulus and filter. |
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To derive completeness functions, SC candidates at fixed magnitudes
are artificially added in the frame on a grid of 100 pixel separation
both in x and y coordinates, the photometry of artificial sources is
then obtained in the same way as for the original data. The comparison
of the input and output photometric catalogues is used to evaluate the
completeness fraction
.
The
experiments are repeated for i) different magnitudes (between 15
and 30 mag, with steps of 0.1 mag), and ii) for different positions
of the grid of stars. The results of the completeness tests are shown
in Fig. 12. The completeness fraction is quite low in
the innermost annulus (#1), though we recall that no source in the
final catalogue lies in such area of high, and highly variable galaxy
background (Fig. 11).
Using the completeness functions so derived, we estimated the
corrected LF of SC candidates, shown in Fig. 13. The
observed sharp falloff is an artifact due to the sample incompleteness
at faint magnitudes. In the three panels of the figure we plot a fit
to the data, the slope
obtained from a power law fit
dN/d
is also reported. To minimise the effect of
incompleteness, the upper limit of the fit is chosen so that the
completeness fraction in the innermost useful annulus, #2, is
. Notwithstanding
the complex issue of completeness, the power law fit to the data
provides exponents
similar to what typically found in
spirals and starburst galaxies
(e.g. Whitmore et al. 1999; Larsen 2002; de Grijs et al. 2003; Miller et al. 1997). We also
find, for all three passbands considered, steeper slopes on the bright
sides of the LFs, with power law exponents as large as
.
In all cases, however, the new exponent agrees within
1
uncertainty with the single power-law slopes reported in the
figure. The presence of a bend in the SCLF has already been found in
various galaxies. As discussed in details by
Gieles et al. (2006a,b), a SC system originating from a truncated
mass function (MF), possibly caused by a truncated MF in the giant
molecular clouds, is expected to show such a bend, with steeper slopes
on bright side of the LF. One other prediction of a truncated MF is
the steepening of the LF at longer wavelengths. In spite of the
uncertainties on the fitted slopes, this behaviour seems to be found
in our data. Nevertheless, comparing maximum cluster luminosity
(
mag) with the number of clusters brighter than
mag (
N(MV<-8.5)=13), as proposed by Gieles et al. (2006a, see also
the references therein), we find that the luminosity of the
brighter cluster in NGC 3370 can be accounted for by a size-of-sample
effect, with a single power-law distribution (see Fig. 16
in Gieles et al. 2006a).
![]() |
Figure 13: Left panel: B-band Luminosity Function of SC candidates. The dot-dashed line shows the power law fit to the data. The exponent of the fit is also reported in the panel. Middle panel: as upper panel, but for V-band data. Right panel: as upper panel, but for I-band data. |
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The consistency of the SCLF with a power law indicates no preferred
scale for cluster luminosity (i.e. mass). However, ``passive''
evolutionary processes like tidal interactions, dynamical friction,
and the ``active'' evolution of stars in the cluster are expected to
alter the shape of the SCLF. On the contrary, the luminosity function
of GCs (GCLF) in both elliptical and spiral galaxies shows a nearly
universal turn-over at
mag (Harris 2001; Richtler 2003),
implying that present GCs have a preferred mass scale. By
inspecting the data in Fig. 13, we do not see any
peculiarity near the regions of the GCLF peaks (
mag, and
mag), although this might well be a consequence of the
poor number of GC candidates in our final catalogue
(Sect. 3.5) and the dominance of young objects.
One more piece of information comes from the study of the
correlation between the SCLF and Star Formation Rate (SFR) of the
galaxy. As shown by different authors
(e.g. Larsen & Richtler 2000; Larsen 2002; Billett et al. 2002), some properties of the SC
system are correlated to the SFR, with the efficiency of cluster
formation being larger in galaxies with higher SFR. In particular,
Larsen (2002) analysed the maximum luminosity expected from a
random sampling of the LF (assuming a power law exponent
)
versus the SFR per unit area. The comparison of
predictions to observations showed a satisfactory agreement. Using the
LF shown in Fig. 13 we find that the maximum observed SC
candidate magnitude is
mag. Assuming the
yr-1 by Grosbøl & Dottori (2008, a ``crude calculation'' based on
the K-band properties of bright knots in the galaxy), and
an area
kpc2, we find that NGC 3370 data fall in the same
observational regions as the spirals in Fig. 16 of
Larsen (2002), without any noticeable scatter with respect to other
observational data. Moreover, the behaviour with respect to the
predictions presented in Larsen (2002), based on sampling
statistics, is offset by nearly the same amount (
0.9 mag, or
0.7 mag, depending on the model) as other spirals.
3.3 About effective radii and spatial distribution
In this section we analyse the
versus various other
characteristics of the SC candidates, or the host environment. Let us
first inspect the
distribution of the system.
Upper panel of Fig. 14 shows the distribution of
using both the radii obtained from the weighted average of V and Ivalues (solid histogram), and those obtained using all BVI data
(dotted line). The differences between the two distributions is
negligible, mainly because the B-band
have larger uncertainties,
thus lower weights. As anticipated, we adopted the V and I averaged
values.
The lower panel of Fig. 14 shows the distribution of
in logarithmic scale. A power law fit to the data (solid line)
for
larger than
3 pc, provides an exponent
.
Such value is consistent with similar results for
other galaxies. For example, Bastian et al. (2005) found
for the star clusters in M 51, although they fit with the same power
law the whole set of
(2 pc
pc). In Fig. 14 it is shown also that a log-normal distribution with a
peak at
3 pc (dotted line) provides a good fit to data.
![]() |
Figure 14:
Upper panel:
|
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The median
of the system is 4.2, with 3.0 pc standard
deviation. If the three possible sub-populations of SC candidates
(Sect. 3.1) are taken separately, we obtain as median and
standard deviation
pc for the
blue/intermediate/red peak, respectively (using only the SC candidates
within 1
the colour intervals reported in Fig. 10,
the number of objects used are 7, 72, and 18 from blue to red
peak
). Although the three
median
agree within 1
,
we notice smaller
for bluer
SC candidates. Figure 15 gives more details on this
regard. In the figure we show the average
per colour bin for
both B-I and B-V. In spite of the large scatter, it is possible to
observe the presence of a non negligible correlation between the size
and the colour of SC candidates, with red SCs showing on average
larger
respect to blue candidates. Such effect has already been
observed in other SC systems (e.g. Scheepmaker et al. 2007). Again, if
colour differences are associated to age differences, then the
increase of
with colour points toward a dynamical evolution of
clusters radii with age, with younger objects being more concentrated
than older ones.
![]() |
Figure 15:
Median
|
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![]() |
Figure 16: Average effective radius versus distance from the galaxy centre. |
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The spatial distribution of star clusters provides an additional piece
of information on the properties and origins of the SC system and the
host galaxy. One possible clue comes from the relation between the
half-light radius and the galactocentric distance
,
shown in
Fig. 16. Also in this case, the spread around the average
for each
bin is large, but a correlation over the
entire
range seems to be present. A linear fit to the data
provides a slope
.
By analysing the SC system of
M 51, Scheepmaker et al. (2007) found a shallower slope,
.
However, similarly to M 51, we find no
correlation, or a very weak one, between the colour of the SC
candidate and
(Fig. 17). Finally, the spatial
density of SC candidates versus
,
shown in Fig. 18, reveals that the surface brightness profile of the
galaxy (in the figure with an arbitrary shift) agrees with the radial
density profile of SC candidates. In the figure we omit the
central
2 kpc as SC candidates in such bright region are
rejected. A linear fit to SC data provides a slope
,
very similar to the
from the surface brightness
profile of the galaxy. Such behaviour, typically observed in late
type galaxies (Larsen 1999; Schweizer et al. 1996; Miller et al. 1997), might be an
indication that field stars and star clusters have experienced similar
dynamical relaxation processes and, that star clusters at any location
(and age?) are in dynamical equilibrium with the galaxy potential.
![]() |
Figure 17: Average colour of SC candidates versus galactocentric distance. |
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3.4 Mass function from comparison with models
Mass estimates of SCs are sensitive to the age of the cluster,
because the mass luminosity ratio changes with time, due to stellar
evolution, and because of the dynamical evolution of cluster itself
(tidal disruption, evaporation, etc.). In the approximation of no
dissolution, Gieles et al. (2007), using SMC data, find that the minimum
detectable cluster mass scales with age t according to
,
or, in other words, the mass detection
limit increases by a factor of
5 each age dex (see
also Boutloukos & Lamers 2003, for a similar analysis on clusters in the MW and nearby
galaxies). As discussed in Sect. 3.1, the present
sample of clusters contains both massive old GCs, which have a peaked
mass function, and young clusters, which form from a power-law mass
function. Therefore, an age dependent mass-completeness affects our
data. To properly constrain the mass of SC candidate, age sensitive
data, like U-band photometry, are essential, and a study of the SC
masses drawn from only BVI data must be considered with extreme
caution.
Keeping in mind these warnings, in this section we tentatively
derive rough mass estimates of SC candidates. To this purpose we use
magnitudes and colours of SC candidates and compare them with stellar
population synthesis models. In particular, we take advantage of the
specific capabilities of the Teramo-SPoT models
(Cantiello et al. 2003; Raimondo et al. 2005), to obtain some hints on the mass distribution of the
SCs. Drawing the mass distribution from a comparison of data to SSP
models is a risky exercise, and could be misleading if one does not
consider properly the limitations due to the assumptions done. The
total mass of the SSP strongly depends on the Initial Mass
Function. We assumed a Scalo (1998) law; a different IMF, like a
Salpeter (1955) or a Kroupa (2001) IMF, would affect the total
mass estimates by few tens percent. However, that's rather unimportant
for the rough, and relative analysis that we will carry out here. A
second approximation comes from the fact that the age and mass
associated to each SC candidate depends on the metallicity of the
stellar cluster. For this reason, we have assumed three metallicities,
representative of metal rich, intermediate, and and metal poor stellar
populations, i.e. [Fe/H]
and 0.0 dex, respectively.
Then, we have analysed the three cases separately.
![]() |
Figure 18: Radial density of SC candidates corrected for completeness (thick solid line). The completeness correction is only significant in the innermost two bins considered. The upper thin solid line shows the surface brightness profile of the galaxy shifted vertically by an arbitrary amount. The slope of a linear fit to both distributions is also reported in the figure. |
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To derive crude mass estimates of the SC candidates we used two different approaches, both based on the data to model comparisons: first we compare SC candidates colour and magnitudes with SSP models for the three selected [Fe/H] separately, then a second estimate of masses is obtained in the colour-colour plane from median mass-luminosity ratios.
For the specific purpose of this work we have computed SSP models
assuming different total masses, i.e.
,
and
ages 0.03, 0.2, 0.5, 1.0, 5.0, 10.0, 14.0 Gyr, for the three adopted
metal contents. The upper panels in Fig. 19 show a
comparison of data to models for the selected [Fe/H] values, all
computed ages and masses are shown.
![]() |
Figure 19:
Upper panels: magnitude-colour diagrams of SC candidates and
SPoT SSP models for the three reference metallicities ([Fe/H] upper
quotes in each panel). Models with ages 0.03, 0.2, 0.5, 1, 5, 10 and
14 Gyr are connected with a line, older ages have redder
colours. SSPs models with different masses,
|
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Assuming a defined [Fe/H], we used the SSP grids shown in Fig. 19 to constrain the mass of the SC candidate, rejecting
all SC candidates that lie outside all SSP grids by more than 0.2 mag. The lower panels of Fig. 19 show the mass
distributions derived from the data-model comparisons described.
![]() |
Figure 20: Upper panel: SC candidates (dots) compared to SSP colour predictions from SPoT for [Fe/H] = -1.8, -0.7, 0.0 (shown with solid, dashed and dot-dashed lines, respectively). The models age ranges from 0.03 to 14 Gyr. Lower panel: the PMF derived from the estimate of median M/LV ratios of SC candidates. |
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Although we cannot give solid constraints on the present mass function
(PMF) of SCs, it is instructive to study some features of the
magnitude-colour diagrams and PMF derived. First, a few very blue
[
mag,
mag] SC candidates can only be
associated to a metal poor and young component, since intermediate
[Fe/H] and metal rich models do not provide the necessary colour spread
to match these sources. Moreover, the position in the magnitude-colour
diagram of these sources implies low masses,
.
This is also recognised by the presence of a peak at
in the PMF at [Fe/H] = -1.8, while the PMF derived
from other [Fe/H] are nearly flat below
.
The
expected age-dependent mass completeness (Gieles et al. 2007) is probably
observed in the panels of Fig. 19, too. In fact, only
young SC candidates overlap with SSP models with masses below
,
while no SC candidate matches with the grid of
low-mass
Gyr SSP models, no matter what [Fe/H] is adopted.
A similar case are the red objects at
,
which can only be
associated to a population of old, metal rich SCs. Although the sharp
drop of the PMFs at masses
might be an artifact
of the sample incompleteness, it is worth to note that in all cases a
turn over of the PMF around
is observed.
Finally, a linear fit to the mass distribution, within the range of
,
provides a slope
that agrees within 1
uncertainty
.
As an additional test we have obtained masses by using the average
mass-luminosity (M/LV) ratios derived from the B-V versus V-Icolour-colour diagram, then converting V-band magnitudes to masses.
More in details, we have constrained the mean M/LV of the SC
candidates by the comparison of SC colours with SSP models in a broad
range of ages (
(Gyr)
)
and [Fe/H] from -2.3 to
+0.3 dex. We set a default 0.25 ``colour distance'' to the SSP model
for accepting its M/LV ratio
. The upper panel of Fig. 20 shows the
colour-colour diagram of SC candidates, and the three reference SSP
models from SPoT. The median M/LV obtained from the data-to-models
comparison was then used, together with visual magnitude of the SC
candidate, to estimate the mass. The main difference with this new
approach is that no a priori assumption is done on the [Fe/H] content. Moreover, in the previous approach, at fixed [Fe/H] the mass
and age of the SC were virtually present in the comparisons shown in
Fig. 19 (upper panels), while in this case mass comes
from the statistical analysis of the M/LV of SSP models within
large age and [Fe/H] ranges. The PMF derived using M/LV ratios is
shown in Fig. 20. Our main interest, here, is to
emphasise that the two approaches used to derive the PMF provide
similar results concerning the power law profile.
The PMF in spiral and irregular galaxies is generally well fit by a power-law,
although the fit is limited to the young and most massive component of
clusters. The typical value for power law exponent is
(e.g. Zhang & Fall 1999; Bik et al. 2003). Similarly, the high mass tail of
Galactic OCs has a slope
,
with no selection on
clusters age, thus including objects from few Myr up to several Gyr
(Battinelli et al. 1994).
Such numbers agree with the slopes obtained from the power-law fit to
data (shown in Figs. 19, 20), ranging
between
and
,
and corresponding to a power
law index
in the form d
/d
.
Recently, Larsen (2009) proposed that the power-law fit to the MF
of SCs might be due to the limited mass range of observational data,
and suggested that a functional form of the type of a Schechter law -
characterised by a power law and an exponential decline after some
characteristic mass
- approximates
quite well some of the best studied SC systems, like in M 51 and
LMC. However, Larsen also warns that it is unlikely
that such functional form is universal, quoting the cases of some
merger or starburst galaxies as examples where significantly higher
values are required. As a non-interacting spiral, NGC 3370
should fall in the sample of galaxies with a PMF well described by a
Schechter form. Assuming a Schecter function as in Larsen (2009), a
cut-off mass of the order of
would be
required for the approximate PMF derived here. Such high
value
has been fit to the young SCs in the Antennae (Jordan et al. 2007), but it
is highly unlikely in spirals, being probably a result of the sample
incompleteness at low masses, and the rough mass estimates used here.
![]() |
Figure 21: Colour histograms of GC candidates in NGC 3370 ( upper panels) and of bright GGCs ( lower panels). The histograms are normalised to the bin with maximum amplitude. |
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3.5 Globular Cluster candidates
The colour distributions of NGC 3370 clusters, and the comparisons
with GGCs, as well as with the cluster system in other galaxies, shown
in previous sections, has evidenced the presence of a red system of
objects with properties remarkably similar to old globular
clusters. In this section we provide a more detailed study on such GC
candidates. To select a sample of candidate GCs we consider only
sources with V-I matching with the GC system in the Galaxy, in
addition sources in the brightest/bluest part of the disk are rejected
to avoid contamination (
,
mag/arcsec2). With such criteria we end up with a list of 35 GC
candidates. Figure 21 shows the colour histograms (normalised
to the maximum bin amplitude) for GCs in NGC 3370 and, for
comparison, for GGCs brighter than
(GGC data
from Harris 1996). The median colours are
mag
(
mag), and
mag (
mag)
for NGC 3370 (MW) star clusters. The median
is
5.5 with
3.9 pc standard deviation. Having in mind the warning of the small
sample of GC selected, it is possible to associate the similarity
between the B-V and B-I colour distributions in both galaxies to
similar age/metallicity properties of the two GC systems. However,
some differences seems to be recognised between the two
galaxies. First, the colour distributions in NGC 3370 do not appear
so sharp as in the case of GGC, though this might be a consequence of
larger photometric uncertainties. Second, both NGC 3370 distributions
show a tail of GC at bluer colours with respect to the MW - more
evident in B-I. If the apparent secondary peak is interpreted as a
metallicity difference then, using the B-I colour-metallicity
relation by Harris et al. (2006) derived from GGCs, we find that the main
peak corresponds to a metallicity [Fe/H]
dex (as for the
Galaxy), while the [Fe/H] for objects in the blue tail is
-2.3dex. However, we must emphasise that several doubts have been raised
in the last few years against the simple interpretation of colour
bimodalities in GC systems as metallicity bimodalities. Non-linear
metallicity-colour transformations, in fact, have been proved to be
effective in generating multimodal colour distributions from unimodal
[Fe/H] distributions (see Cantiello & Blakeslee 2007, and references therein).
One other useful quantity related to the GC system is the specific
frequency, SN, i.e. the number of GC normalised to the host galaxy
luminosity. This number provides a useful quantity related to the
formation mechanisms of the galaxy (see Brodie & Strader 2006, and references
therein). To properly estimate SN, however, the total
number of GC needs to be used. As a consequence of the sample
incompleteness we cannot reliably constrain the specific frequency,
but only provide an estimate to the lower limit of SN. In
particular, we make the following assumptions: i) we use the results
by, e.g., Rhode & Zepf (2003) showing that the surface density of GC in
spirals follows a power law profile; ii) a total apparent corrected
magnitude
mag for NGC 3370 from
Hyperleda
is adopted, and iii) a
the slope for the density profile of
is fixed from the compilation of Kissler-Patig (1997), for a total
galaxy magnitude
mag. By constraining the intercept of
the density profile from the number of GCs within
- corrected for photometric completeness - we
find a lower limit of
,
to be compared with
for the GC systems on other spirals (Kissler-Patig 1997; Chandar et al. 2004; Rhode & Zepf 2003).
4 Summary
Deep optical VI and shallower B band observations of the face on spiral galaxy NGC 3370, drawn from the ACS/HST archive, have been used to study the SC system in the galaxy. The characteristics of the imaging data available allowed to analyse the photometry of SC candidates, and their spatial properties. The final list of SC candidates consists of 277 objects, selected according to maximum colour, magnitude, size and position within the galaxy.
The analysis to the sample of SC candidates leads to the following conclusions:
- (1)
- The colour distributions show that the SC population is composed
by different subpopulations. In particular, the differences are
related to ages, with the main sub-populations represented by i)
a red system of likely GC candidates; ii) a dominant peak of
sources with properties similar to intermediate age clusters
(similar to OCs with ages from a few 100 Myrs, to few Gyr); and
iii) a blue tail of SCs, possibly with ages below
100 Myr. Such complex age-structure of the SC system is somehow expected in a Sc-type spiral, actively star-forming (as also testifies the amount of Cepheids observed in this galaxy).
- (2)
- The comparison of SC candidates colours - selected with no a
priori assumption on the range of colours allowed - with SSP
models predictions within a large range of ages (30 Myr to 14 Gyr)
and [Fe/H] (-2.3 to +0.3 dex) shows a good matching between models
and data. A significant exception to this is represented by a
sample of
20 SC candidates, which systematically lie outside the region of SSP models, showing an excess of flux at longer wavelength (I-band magnitude). Such SC candidates do not show remarkable peculiarities in terms of spatial distributions or morphology. One possible origin of their behaviour is that they are typical intermediate age SCs (300 Myr to 2 Gyr). At these ages, the stochastic presence of TP-AGB stars has a dramatic impact on the integrated light. In particular, TP-AGBs dominate the long-wavelength emission of the stellar system (see, e.g., Maraston 2005; Marigo et al. 2008, and references therein), thus the stochastic presence of TP-AGBs might cause the observed position of these SCs in the colour-colour diagram (Raimondo 2009).
- (3)
- The median
of the system is 4.2 with 3.0 pc standard deviation. The
distribution shows a power law drop above
pc. The exponent of the power law,
, appears normal with respect to other similar galaxies. Moreover, a log-normal fit to the distribution of
seems to show a turn-over around
3 pc, although the completeness of the data does not allow to give more robust conclusions.
- (4)
- The
shows non-negligible correlations both with the colour of the SC candidate, and with the galactocentric distance Rgc. If colours differences are associated to age differences, as suggested in (1), these results point toward an age evolution of
, with older SCs having larger
. Furthermore, the spatial density of clusters, which appears similar to the surface brightness profile of the galaxy, might well be a consequence of a common dynamical evolution of stars and star clusters in the gravitational potential of the galaxy.
- (5)
- The LF of SC candidates shows a continuous increase down to
magnitudes where the SC candidate sample is fairly unaffected by
incompleteness. Such LF is well described by a power law with
exponent slightly below
-2.0 in all bands. This functional form agrees to that of other SC systems in spiral or irregular galaxies. A comparison of the maximum SC magnitude with the SFR per unit area shows that the correlation between these quantities is like in other spirals. Moreover, some properties of the LFs presented here (steepening of the LF towards brighter magnitudes, and steeper slopes at longer wavelengths) seem to support the idea that the SCLF is originated by a truncated mass function, though sample incompleteness hampers more detailed conclusions.
- (6)
- By comparing data to SSP models, we tentatively derived a crude
estimate of the Present Mass Function of the SC system. Since our
data suffer for the lack of an age-sensitive indicator, the PMF
derived must be taken carefully as a best guess with available
data. With this warning in mind, we find that a power law fit to
the interval of more massive SCs (i.e. objects likely less
affected by the incompleteness) provides an
, in agreement to what can be found in literature for similar galaxies. Moreover, the PMF seems to show a turn-over around masses of the order of
, though this is possibly due to the sample incompleteness at lower masses.
- (7)
- We analysed the properties of a sample of GC candidates, selected
on the base of their V-I colour, and their positions with
respect to the centre of the galaxy. The number of GC candidates
selected is 35, these show colour distributions similar to GGCs,
though less peaked around a median value (probably due to the
larger photometric uncertainties), and with a relatively more
populated tail towards bluer colours. The peak of the colour
distribution, converted to metallicity using GGCs data, gives
[Fe/H]
-1.5, similar to GGCs.
- (8)
- Due to the complex issue of completeness in these data, we cannot provide a reliable estimate to the specific frequency of GCs. However, taking advantage of the known approximative behaviour of the surface density profile of GC in spirals, we estimate a lower limit SN>0.8.

Acknowledgements
It is a pleasure to thank Gabriella Raimondo for several scientific discussions and for her irreplaceable support in computing theoretical models. We are also grateful to Sören Larsen for his fruitful comments and suggestions on data analysis. Part of this work was supported by PRIN-INAF 2006 (PI G. Clementini). We would thank the referee, Dr. Mark Gieles, for valuable remarks and suggestions.
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Footnotes
- ... NGC 3370
- Full Table 3 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/503/87
- ... 4 pixels
- The
alignment between single HST frames is generally better than the
maximum wandering adopted here. Our choice has been motivated by the
large spatial variability of NGC 3370 surface brightness profile, and
its wavelength dependence, which may lead to different estimates of
the source centroid in different bands. A posteriori, we verified that
for none of the SC candidates in the final sample the coordinate
wandering between V and I frames exceeds
2 pixels.
- ...=28.5 mag
- The aim of the selection based on the
SExtractor morphological parameters CLASS_STAR, and A_IMAGE/B_IMAGE
is to remove from the candidate list all obvious non SCs. Visual
inspection of objects rejected in this way revealed that they are
mostly extended, irregular, diffuse or elongated objects. Moreover, in
a further selection based on ishape output parameters (see end of this
section), we rejected candidates with elongation estimated by ishape
2. The limiting magnitudes adopted here are, instead, related to the S/N ratio of ishape. Tests made on sources fainter than the limiting magnitudes adopted showed that the S/N is in all cases much lower than the minimum acceptable value
30 suggested by Larsen (1999).
- ...
IRAF
- IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.
- ... objects
- The complete catalogues of sources can be retrieved upon request to the authors.
- ... 11 OCs)
- Ages and colours for OCs are from the WEBDA database, available at http://www.univie.ac.at/webda
- ...
- The average f between annuli #2, #3, and #4 at the faint limit is larger than 0.8 in all bands.
- ...
peak
- We obtain
pc for the blue/intermediate/red peak using SC candidates within 2
the colour intervals of Fig. 10.
- ...
) - Visit the website www.oa-teramo.inaf.it/spot for details on models, code, and for downloads.
- ... uncertainty
- The lower limit to
has been chosen to avoid the masses, i.e. magnitudes, most affected by incompleteness. The B-band completeness at masses approximatively lower than
drops quickly below 90%.
- ... ratio
- We made several tests using different ranges (from 0.1 to 0.5 mag, also releasing the matching between colours), without any substantial change in the PMF slope.
- ...
Hyperleda
- http://leda.univ-lyon1.fr
All Tables
Table 1: NGC 3370 properties and observations.
Table 2: Number of objects rejected per selection criteria.
Table 3: Structural and photometric properties of selected SC candidates. The full table is only available in electronic form at the CDS.
All Figures
![]() |
Figure 1:
ACS B, V and I composite image of NGC 3370, the image size is
roughly
|
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Upper to lower panel: radial I, V and B band surface
brightness profiles of NGC 3370. The linear fit to the data at
|
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Central panel: effective radii from the I-band frame versus
the V-band
|
Open with DEXTER | |
In the text |
![]() |
Figure 4: Some examples of visual classifications codes. For each source we show the original I-band image ( upper sub-panels) and the ishape residuals ( lower sub-panels). Objects associated to the classes 33 (large residuals, crowded area), 100 (possible background galaxies), and stars are rejected in the final catalogue of SC candidates. |
Open with DEXTER | |
In the text |
![]() |
Figure 5: Aperture corrections in B, V, and I-band versus the SC candidate radius. The solid lines show the best fit linear equation. |
Open with DEXTER | |
In the text |
![]() |
Figure 6:
Colour-colour diagram of the SC candidates. Dark-grey dots,
empty and full circles mark the positions of the sample after the
first, second and third (final catalogue) selections described in
Table 2. The grey shaded area marks the region of
SPoT-SSP models by Raimondo et al. (2005). The arrow shows the direction of the reddening
vector. Five pointed stars are ``outlier'' SC candidates, possibly
associated to intermediate age clusters. The insert
panel shows the SC candidates (full dots), the SC outliers
(five-pointed stars), and the standard SPoT SSP models (grey-shaded
area). The dark-grey area shows the region occupied by SSP realisations
of the recent SPoT models by Raimondo (2009), computed paying
particular attention to the stochastic effects of TP-AGB stars. Only
ages between 0.3-2 Gyr and [Fe/H] |
Open with DEXTER | |
In the text |
![]() |
Figure 7: Left panels: B-V colour magnitude diagram ( upper panel) and colour histograms ( lower panel) of SC candidates. Right panels: as left, but for B-I. The arrows indicate the median colour of GGCs. |
Open with DEXTER | |
In the text |
![]() |
Figure 8:
Colour histograms of the comparison galaxies (as labelled in
left panels). Dotted lines show NGC 3370 SC candidates. For NGC 3367
and SMC a different binwidth is used, because of the smaller number of
SCs (see
|
Open with DEXTER | |
In the text |
![]() |
Figure 9:
B-V colour histograms of LMC Star Clusters (solid lines)
and NGC 3370 (dotted lines). The vertical blocks refer to LMC
clusters selected according to the SWB class: the first, second and
third row refer to LMC clusters with SWB
|
Open with DEXTER | |
In the text |
![]() |
Figure 10: Upper panels: colour histograms of SC candidates, the position of the three relative peaks is emphasised in each panel with dashed lines. Lower-left panel: spatial distribution SC candidates selected according to their membership to the colour sub-peaks (see text). Five pointed stars/full squares/circles mark candidates in the blue/intermediate/red tail respectively. |
Open with DEXTER | |
In the text |
![]() |
Figure 11:
Annuli division used to compute completeness functions. The
regions are characterised by their median surface brightness:
|
Open with DEXTER | |
In the text |
![]() |
Figure 12: B, V and I-band completeness functions for the each of the four annuli considered (labelled in the panels). For each one of the 4 annuli, we have carried out several numerical experiments shifting the grid of artificial stars. Different experiments are shown with different line types in each panel. The horizontal dotted line marks the 90% completeness limit in the annulus. The rightmost panels show the median completeness function for each annulus and filter. |
Open with DEXTER | |
In the text |
![]() |
Figure 13: Left panel: B-band Luminosity Function of SC candidates. The dot-dashed line shows the power law fit to the data. The exponent of the fit is also reported in the panel. Middle panel: as upper panel, but for V-band data. Right panel: as upper panel, but for I-band data. |
Open with DEXTER | |
In the text |
![]() |
Figure 14:
Upper panel:
|
Open with DEXTER | |
In the text |
![]() |
Figure 15:
Median
|
Open with DEXTER | |
In the text |
![]() |
Figure 16: Average effective radius versus distance from the galaxy centre. |
Open with DEXTER | |
In the text |
![]() |
Figure 17: Average colour of SC candidates versus galactocentric distance. |
Open with DEXTER | |
In the text |
![]() |
Figure 18: Radial density of SC candidates corrected for completeness (thick solid line). The completeness correction is only significant in the innermost two bins considered. The upper thin solid line shows the surface brightness profile of the galaxy shifted vertically by an arbitrary amount. The slope of a linear fit to both distributions is also reported in the figure. |
Open with DEXTER | |
In the text |
![]() |
Figure 19:
Upper panels: magnitude-colour diagrams of SC candidates and
SPoT SSP models for the three reference metallicities ([Fe/H] upper
quotes in each panel). Models with ages 0.03, 0.2, 0.5, 1, 5, 10 and
14 Gyr are connected with a line, older ages have redder
colours. SSPs models with different masses,
|
Open with DEXTER | |
In the text |
![]() |
Figure 20: Upper panel: SC candidates (dots) compared to SSP colour predictions from SPoT for [Fe/H] = -1.8, -0.7, 0.0 (shown with solid, dashed and dot-dashed lines, respectively). The models age ranges from 0.03 to 14 Gyr. Lower panel: the PMF derived from the estimate of median M/LV ratios of SC candidates. |
Open with DEXTER | |
In the text |
![]() |
Figure 21: Colour histograms of GC candidates in NGC 3370 ( upper panels) and of bright GGCs ( lower panels). The histograms are normalised to the bin with maximum amplitude. |
Open with DEXTER | |
In the text |
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