- Original article
- Open Access
Growth and reproductive biology of the sea star Astropecten aranciacus (Echinodermata, Asteroidea) on the continental shelf of the Catalan Sea (northwestern Mediterranean)
Helgoland Marine Research volume 70, Article number: 1 (2016)
The growth and reproductive biology of the sea star Astropecten aranciacus was investigated on the continental shelf of the northwestern Mediterranean Sea. Sea stars were captured monthly in two bathymetric ranges (5–30 and 50–150 m) between November 2009 and October 2012. Bathymetric segregation by size in A. aranciacus was detected: small individuals inhabit shallow areas (5–30 m), while large individuals inhabit deeper areas of the continental shelf (50–150 m). Recruitment was recorded twice nearshore but no recruitment was detected offshore during the whole study period. Three cohorts were identified in each bathymetric range and growth rates were estimated. A. aranciacus population exhibited a seasonal growth pattern, being higher from June to October in the nearshore cohorts and from February to October in the offshore ones. Histology and organ indices revealed that spawning likely started in March, coinciding with the spring phytoplankton bloom and the increase in sea water temperature, and extended until June–July. Ratio between males and females was approximately 1:1 throughout the year and in both bathymetrical ranges. The size at first maturity (R50 %) was estimated to be R = 112 mm. A. aranciacus did not show an inverse relationship between gonad index and pyloric caeca index.
Sea stars play an essential ecological role as high-level predators in the structure and function of intertidal and subtidal benthic communities, where they promote heterogeneity and diversity . Changes in the abundance of these predators can have far-reaching consequences on the population characteristics of many of the invertebrates on which they prey . Despite the ecological importance of sea stars, research has been mainly limited to certain species and to areas where they have an economic impact because they feed on important shellfish or on reef-building corals .
Astropecten (Fam. Astropectinidae) is one of the most species-rich genera among sea stars and its members are distributed worldwide, from polar to tropical seas and from intertidal areas to the deep sea . They are voracious predators, feeding mainly on gastropods and bivalves. They have an intra-oral feeding mechanism, swallowing prey intact . In general they exhibit a patchy spatial distribution as a consequence of a combination of biotic (e.g., prey and congener abundance) and abiotic factors (e.g., depth and sediment properties) . Astropecten spp. have a pair of gonads and a pair of pyloric caeca (digestive organs) located in each arm . Gonad and pyloric cecum indices are widely used as indicators of reproductive effort and nutritional condition. Resources stored in pyloric cecum seem to play an important role in the seasonal production of gonads in some asteroid species .
There is a vast literature on the genus Astropecten worldwide, mainly focusing on their feeding behavior, diet characteristics [3, 11] and early stages of development [22, 27]. However, aspects of their biology such as growth and reproductive biology have been less analyzed than those of other sea star genera . Growth in field populations has been studied in both tropical  and temperate waters [15, 35]. Ventura  observed a growth decrease coinciding with the seasonal upwelling season in Brasil. Freeman et al.  observed that A. irregularis growth in North Wales was highly seasonal, with maximum growth occurring between mid-summer and mid to late autumn. Ventura  Astropecten spp. reproduction has been analyzed in temperate [11, 15, 18] and in tropical waters [31, 47, 48]. Reproduction is usually seasonal in temperate waters and spawning takes place with the increase in water temperatures ; however, in tropical waters sympatric Astropecten species seem to react differently to changes in sea water temperature and then, spawning occurs at different seasons .
Astropecten aranciacus (Linnaeus 1758) inhabits the Mediterranean Sea and the eastern Atlantic from Portugal to Angola, including the Canary, Madeira and Cape Verde Islands. It is one of the largest sea stars in the Mediterranean Sea, with a body diameter of up to 60 cm. It lives on sandy, muddy and detrital bottoms, as well as on seagrass beds, including Zostera, Cymodocea and Posidonia, between 1 and 200 m depth . A. aranciacus is the dominant species on the continental shelf of the Maresme coast (northwestern Mediterranean Sea), where it co-occurs with other species of the same genus (A. platyacanthus, A. irregularis pentacanthus, A. bispinosus, A. spinulosus and A. jonstoni) between 5 and 30 m depth . Baeta and Ramón  observed that Astropecten sea stars have niche segregation, showing a partitioning of the resources and occupying different microhabitats to avoid food competition. At depths between 50 and 200 m in the same area, A. aranciacus co-occurs with A. irregularis pentacanthus and other non-congeneric species (Luidia ciliaris, Tethyaster subermis, Peltaster placenta, Anseropoda placenta and Hacelia attenuata) .
Astropecten aranciacus has a defined behavioral pattern: it remains buried in the sand during the daytime, emerges just before sunset and looks for prey all night, and buries itself again just a few hours after dawn . In the study area A. aranciacus feeds mainly on the bivalves Glycymeris glycymeris and Callista chione, together with the gastropod Cyclope neritea between 5 and 30 m depth ; and almost exclusively on the bivalve Timoclea ovata between 50 and 200 m depth . Recently, a major decrease in its population has been detected in the Mediterranean Sea .
This paper examines for the first time growth and reproduction aspects of A. aranciacus. For this purpose, we have analyzed modal progression of size classes, histological sections of gonads and variations of the pyloric caeca and gonadal indices. In addition, the influence of exogenous factors such as photoperiod, sea water temperature and chlorophyll (Chl a) concentration on the reproductive biology of the species was also analyzed.
The study was carried out on the continental shelf of the Catalan Sea (northwestern Mediterranean), between the Tordera River delta (northeast) and the mouth of the Tiana seasonal stream (southwest) (Fig. 1). This area is called the Maresme coast, and it is a reflective, sandy and straight, wave-dominated plain which displays a NE–SW trend. The continental shelf has a mean width of 21 km and a gradient of between 0.01° and 10°, with the shelf break occurring at 130 ± 20 m . Its seabed consists of coarse to medium sandy bottoms nearshore and mud and/or sandy bottoms offshore .
Monthly samples were obtained on the Maresme coast between November 2009 and October 2012. Sampling was performed by fishermen on board two vessels from the Arenys de Mar harbor fishing fleet, which use commercial fishing gears according to their fishing modality (shellfish and trawlers) and fishing grounds. The impossibility of sampling the whole study area with the same gear due to local fishing regulations forced us to subdivide the study site into two nearby areas (Fig. 1): nearshore, where the shellfish fleet operate between 5 and 30 m depth; and offshore, where trawlers are allowed to operate below 50 m depth. The strip between 30 and 50 m depth is not covered by these fishing boats in their daily activities. The nearshore area was sampled during daylight onboard the artisanal fishing boat Esparta (10 m in length; 100 hp), which belonged to the smooth clam fishery fleet and used clam dredges. The clam dredge consisted of a metal frame (mouth length, 70 cm; mouth height, 53 cm), a toothed lower bar and a rectangular metal grid box (mesh size, 29 × 29 mm). Each tow lasted approximately 30 min at a speed of 1–1.2 km, and the mean towed area was around 800 m2. The offshore area (between 50 and 150 m depth) was sampled during daylight onboard the small trawl fishing boat San Benito (10.75 m in length; 105 CV), which targeted black bellied angler (Lophius budegassa) and royal sea cucumber (Parastichopus regalis). The trawl net was cone-shaped, with a mouth 4 m wide × 0.5 m high and a quadrangular mesh size of 40 × 40 mm. Each tow lasted approximately 2 h at a speed of 1.8–2 km. All the A. aranciacus caught, regardless of the gear used, were transported in a cool box (4 °C) to the laboratory, where they were weighed and measured. The length of the sea stars was defined as R, major radius length or distance from the center of the oral disk to the tip of the longest arm, and was measured using calipers to the nearest 0.1 mm.
Length–weight relationship was estimated by combining biometrical data from individuals collected monthly between November 2009 and October 2012 in both bathymetrical ranges. The relationship between the length and weight of one organism is usually expressed by the equation W = aL b, where W is body weight (g), L is length (cm), a is the intercept and b is the allometric coefficient. Values of b significantly different from 3 indicated that growth in weight is relatively faster than growth in length (positive allometry b > 3) or lower (negative allometry b < 3).
Nearshore and offshore samples were analyzed separately to study growth due to the different gear selectivity. Sea star length (R) was categorized into 20-mm classes and grouped every 2 months to obtain bimonthly length-frequency distributions. Growth was estimated from the modal class progression analysis in the length-frequency distributions, using the Bhattacharya method , previously used to examine growth in other asteroids [7, 30] and included in the FISAT II software . The parameters of the von Bertalanffy growth function (L t = L ∞(1–e –k (t−t0))) were estimated by nonlinear regression using the FiSAT II software package, where, from left to right, L t is the predicted length at time t (mm), L ∞ is the asymptotic length (mm), k is the growth constant (year−1), t is the age (year) of the A. aranciacus, and t 0 is the age at which L t = 0 .
All nearshore and offshore individuals collected monthly, from May 2011 to September 2012, were used for reproduction analyses. Each sea star was damp-dried and weighed to the nearest 0.001 g. The oral surface was opened by separating the plates along the ambulacral grooves to expose the viscera. The number of immature individuals was annotated, and all gonads from adults were examined (between 18 and 34 gonads per month). Gonads and pyloric caeca of the five arms were removed, damp-dried and weighed to 0.001 g accuracy. Gonads were fixed in 10 % formalin for 24 h, cleaned with deionized water and preserved with 70 % ethanol. The gonad tissue was dehydrated in graded ethanol, and then infiltrated and embedded with glycol-methacrylate resin. Gonads were cut into 4-µm sections and stained in Lee’s methylene blue-basic fuchsin. Microscopic examination of the sections allowed sex determination and assignation of each individual to a gonad maturation state. Development was divided into five stages based on an adaptation of scales used for other asteroid species, where each stage is determined according to the frequency and characteristics of gametes, presence of phagocytes and cell remains, as well as thickness and shape of the gonadal wall [4, 9, 10, 32, 38].
The gonadal index (GI) and the pyloric caeca index (PCI) were calculated as :
Size at first maturation (size at which gonads of 50 % of the individuals are mature, R50 %) was calculated by plotting the percentage of individuals with mature gonads versus size . To analyze the influence of some exogenous factors on the reproductive biology of this species, surface water temperature was obtained from the Barcelona buoy of “Puertos del Estado” (41.32°N/02.20°E), photoperiod data from the “Instituto Geográfico Nacional, Ministerio de Fomento” and the monthly Chl a concentration was obtained from MODIS satellite imagery, using a resolution of 4 km with 0.1 × 0.1 degrees areas.
Sex ratio was tested using a Chi-square (χ 2) test. Differences in the mean gonadosomatic index values between sexes were assessed for each month using a Mann–Whitney U test. A Kruskal–Wallis nonparametric ANOVA was used to check for differences in pooled GI and PCI data among months. Relations among PCI, temperature, photoperiod and Chl a (independent variables) with the reproductive cycle represented by GI (dependent variable) were assessed through a step-by-step multiple linear regression analysis (GLM) using STATA v1.2 statistical Software (Stata Corporation, College Station, TX, USA). Statistical significance was accepted at p < 0.05 .
Sea stars collected from both nearshore and offshore areas had different size compositions (Fig. 2). A. aranciacus major radius length (R) ranged between 11 and 214 mm in nearshore samples, with a mean size of 81.40 mm (SD = 39.44), whereas R ranged between 47 and 280 mm in offshore individuals, with a mean size of 161.33 mm (SD = 44.47). The length–weight relationship can be expressed as W = 0.0025L 2.22 (R 2 = 0.95; F (1.487) = 10,179, N = 1365). Concerning shape variation, the length weight relationship revealed that weight is negatively allometric with length (p < 0.001, t = 35.54), i.e., A. aranciacus becomes relatively more slender as it grows.
The A. aranciacus bimonthly length-frequency distributions at both bathymetrical ranges are shown in Fig. 3. Recruitment nearshore was recorded twice in the whole period of study, in February 2010 and in April 2012. No recruitment or individuals smaller than 100 mm were found in the offshore samples. The progression of the identified cohorts over the 3 years of study can be seen in Fig. 4. In the nearshore samples (Fig. 4a) a cohort (C-1) was observed from April 2012 (R = 47.56 mm) to August 2012 (R = 69.15 mm). Another cohort (C-2) was observed from February 2010 (R = 34.40 mm) to October 2012 (R = 123.62 mm), with a size increase of 89.22 mm. A third cohort (C3) was detected from December 2009 (R = 113.02 mm) to June 2010 (R = 115.51 mm). In the offshore samples (Fig. 4b), we also observed three cohorts. The C-4 cohort was observed from December 2010 (R = 103.04 mm) to October 2012 (R = 144.65 mm); another cohort (C-5) was found from December 2009 (R = 125.58 mm) to August 2012 (R = 171.08 mm); and the last one (C-6) was occasionally detected from February 2011 (R = 206.5 mm) to April 2012 (R = 217.64 mm). Growth rates could be obtained following the mean length of the long lasting cohorts C-2, C-4 and C-5 over time. The nearshore C-2 cohort showed higher growth rates during summer and autumn (18–24 mm from June to October) in the 3 years studied. The offshore cohort C-4 showed higher growth between February–August 2011 (22.8 mm) and February–October 2012 (10.65 mm). The offshore cohort C-5 showed higher growth between April and August 2010 (14.44 mm). The estimated von Bertalanffy growth parameters for nearshore individuals were L ∞ = 136.75 mm, k = 0.44 year−1 and t 0 = 0.0017 (N = 741; R 2 = 0.73), whereas for offshore individuals they were L ∞ = 205 mm, k = 0. 32 year−1 and t 0 = 0.0011 (N = 624; R 2 = 0.82).
Gonads morphology and development
The reproductive system of A. aranciacus comprises two separate gonads in each arm (ten gonads in total). Each gonad was arranged as a series of tufts, located in and attached to the proximal part of each arm, near the disk on the inner face of the lateral wall, below the pyloric caeca, suspended in the celom along the entire length of the arm. Mature gonads were pale cream in males and deep yellow in females. The gonadal wall consisted of two-sac structures (the inner and the outer sacs) separated by the genital celom, which is typical for asteroids.
The five stages that characterize the gonadal development of A. aranciacus are the following:
Ovogenesis (Fig. 5). I-Recovery Stage Ovaries’ lumen was partially filled with amorphous material, cell debris and phagocytes. The gonadal wall was thick, and the two-sac structures were evident; at advanced recovery stage the surface of the germinal epithelium was lined with oogonia and sometimes with early vitellogenic oogonia (Fig. 5a). II-Growing Stage Early in the growing stage (Fig. 5b), the ovarian surface epithelium was thick and mainly covered by previtellogenic oocytes, although some early vitellogenic oocytes could also be found. Late in the growing stage (Fig. 5c), the ovarian surface epithelium appeared thinner, oocytes accumulated in the lumen and vitellogenic oocytes were dominant. Oocytes showed an eccentric nucleus (Fig. 5c). The cytoplasm of the oocytes appeared blue together with oogonia, whereas the nuclei were stained in pink. III-Mature Stage Ovaries were densely packed and stacked with fully grown oocytes in the lumen, and the surface epithelium appeared thin. Oogonia and previtellogenic oocytes were uncommon and restricted to the germinal layer. The gonadal wall was the thinnest observed in the whole reproductive cycle (Fig. 5d). IV-Partly Spawned Stage Ovaries were poorly packed with fully grown oocytes in the lumen with large empty spaces; previtellogenic oocytes were scarce and not exclusively restricted to the germinal layer. Relict oocyte debris and phagocytes were present in the lumen. The ovary wall remained thin (Fig. 5e). Sometimes atresia was observed. V-Spent Stage Ovaries were filled with amorphous material with relict oocytes, the gonadal wall became thicker, and the two-sac structure was more evident. Relict oocyte debris and phagocytes were present in the lumen (Fig. 5f).
Spermatogenesis (Fig. 6). I-Recovery Stage Testes were small and remained contracted; the lumen was almost empty and partially filled with nutritive phagocytes; the gonadal wall was thick; and the two gonadal sacs were visible. Spermatogenic columns (consisting in spermatogonia) started to develop and grow (Fig. 6a). II-Growing Stage The testes had an intense spermatogenesis activity; they started to widen and became larger. Early in the growing stage, spermatogenic columns were projected into the central lumen and filled almost the totality of the volume; the gonadal wall began to shrink. As the growing stage progressed, testes enlarged and the number of spermatozoa increased from the border of the columns to the central lumen; at the same time the spermatogenic columns became larger as the gonadal wall shrank (Fig. 6b, c). III-Mature Stage Testes were densely packed and compressed with spermatozoa in the lumen, surrounded by very thin spermatogenic epithelium of spermatogenic columns. The wall of the testes was the thinnest observed in the whole reproductive cycle (Fig. 6d). IV-Partly Spawned Stage Testes looked similar to those in the mature stage but spermatozoa were poorly packed; there were spaces between patchy concentrations of spermatozoa in the lumen. Sometimes a gap between the peripheral spermatogenic layer and the central mass of spermatozoa was visible. The gonadal wall became thicker, and inner and outer sacs were visible again (Fig. 6e). V-Spent Stage Testes shrank and became smaller and contracted; the lumen was almost empty, with some nutritive phagocytes and isolated spermatozoa. The wall was thick and the two gonadal sacs became evident (Fig. 6h).
Results showed that females in Stage I (Recovery) were present throughout the study. Ovaries in Stage II (Growing) were also found all year round except in spring (May 2011 and from March to May 2012) (Fig. 7a). The proportion of females with ovaries in Stage II began to increase in June for both study years, and the maximum frequency of occurrence (90 %) was recorded in September 2011. Accordingly, females with mature gonads (Stage III) were observed from October 2011 to May 2012, and most mature females (>40 %) were recorded between February and April. Partially spawned gonads (Stage IV) were observed from December to June, with the highest frequency being found in May 2012. The majority of the spent ovaries (Stage V) were found between March and July for both 2011 and 2012.
Similarly to females, males in Stage I (Recovery) were present throughout the study except for March 2012. Spermatogenesis (Stage II) started between August and September and lasted until January, but was dominant between October and December (Fig. 7b). In accordance, mature testes (Stage III) appeared afterward and were observed in some individuals from December to May. Partially spawned (Stage IV) individuals were found between January and July, with a higher frequency in April 2012. Though a few spent testes (Stage V) were observed in February 2012, most of the individuals in this reproductive stage were observed from March to August.
Sex ratio and size at first maturity
Sea stars did not show sexual dimorphism. A total of 312 individuals were collected from nearshore (87 females, 89 males and 136 immature) and 253 individuals from offshore (135 females, 116 males and 2 immature). The Chi-square (χ 2) test did not show significant differences between sexes; the ratio between males and females was almost 1:1 throughout the year in both bathymetrical ranges: nearshore (χ 2 = 10.186 df = 15; p > 0.05) and offshore (χ 2 = 19.856; df = 16, p > 0.05). The size of the smallest sea star with gonads was R = 56 mm for females and R = 55 mm for males. The size at first maturity (R50 %) was estimated to be R = 112 mm considering both sexes together.
No significant differences between sexes were found when the monthly gonadal and pyloric caeca indices were compared (Mann–Whitney, p > 0.05); values for both sexes were then pooled for further analyses. The gonadal index increased from 0.18 ± 0.24 in Stage I (Recovery) to a maximal value of 5.6 ± 4.42 in Stage III (Mature) (Fig. 8). Once spawning occurred, the GI values declined progressively from Stage IV (Partly spawned) (3.52 ± 2.44) to Stage V (Spent) (0.43 ± 0.44). GI values for A. aranciacus showed significant differences between months (H = 110.07; df = 16, p < 0.001) (Fig. 9). Monthly values revealed an increase from October 2011 to March 2012, when GI reached its maximum (3.62 %). After that peak it decreased until July 2012 (0.14 %). Significant differences were also observed among months for pyloric caeca index (H = 58.76; df = 16, p < 0.001). The highest PCI values were recorded between March and May 2012 (>4.5 %), whereas the lowest were recorded in the summer months (June, July, August 2011, and July, August, September 2012). The surface sea water temperature (SSWT) at the study site had maximum values in summer months (July–September) and minimum values in winter months (January to March) (Fig. 10). Chl a monthly values recorded during our study period were lower between July and September, and two peaks were recorded: one in December 2011 (0.46 mg m−3) and one in March 2012 (0.93 mg m−3). The multiple regression analysis of GI with respect to the PCI and environmental variables was performed in two steps, resulting in the following model: GI = 0.90 + 0.09PCI − 0.03SSWT. The model showed that the total explained variance over the GI in terms of the selected variables was 84.58 % (R 2 = 0.8458, R = 0.88, p < 0.05), indicating that the PCI and surface sea water temperature (SSWT) are correlated with GI. The photoperiod and Chl a did not show any correlation with GI; however, the spawning season coincided with the time period of highest levels of Chl a.
Astropecten aranciacus individuals smaller than 80 mm were abundant in shallow waters (5–30 m depth), whereas large individuals (>130 mm) were observed mostly offshore (50–150 m depth). The use of different gears to sample both bathymetric ranges in this study may have caused bias collecting small sizes offshore, but no bias for larger sizes in shallow waters could occur. Therefore, any bigger individuals of A. aranciacus inhabiting depths between 5 and 30 m would have been collected in our sampling. Burla et al.  studied the activity pattern of A. aranciacus by scuba diving in Sardinia (Italy) and found only small specimens. These authors suggested that adults and juveniles may dwell in different parts of the ecological zone occupied by the species, the fully grown specimens invading the deeper waters. Our study is the first to sample most of the bathymetrical distribution range of A. aranciacus, allowing us to confirm a bathymetrical segregation related to size in this species. Ventura and Fernandes  reported size-depth trends for Astropecten brasilensis in Cabo Frio, Brazil, where they found larger individuals with depth. Segregation by size were also reported for the asteroid Protoreaster nodosus, whose large specimens were found between 0 and 33 m depth, whereas small specimens were exclusively found in shallower habitats (<5 m) . Young sea stars might prefer shallow areas where food and shelters to avoid predation are usually more abundant .
The major radius length–weight relationship showed a negative allometry in A. aranciacus, thereby they invest more energy in body enlargement than in fattening, as previously observed in other Astropecten species [19, 46] and sea stars genera [6, 7]. Absolute growth has been extensively analyzed in sea stars (see references in Lawrence and Lane , but few studies have established growth rates in natural populations of the genus Astropecten [15, 35, 40, 43] (Table 1). The studied A. aranciacus population exhibited a seasonal growth pattern, slightly different for nearshore and offshore cohorts. Individuals living offshore had a longer growth period but their growth rate was slower, as is expected in older specimens. Seasonal variation in growth had been described for other Astropecten species, which usually showed a decrease in growth rate associated with gonad maturation [15, 35, 43]. According to our study, the growth rate for A. aranciacus seems to be related to sea water temperature as higher growth rates were recorded nearshore when sea water temperature was also higher. Moreover, sea water temperature increased slightly from February to December offshore, coinciding with the period of highest growth rate for those cohorts. Ventura  reported that the decrease in growth rate of A. brasiliensis and A. cingulatus coincided with the seasonal upwelling period in Brazil, suggesting that it could be related to sea water temperature decline. Other factors such as the amount and quality of available food can also affect growth, as reported by Guillou and Guillaumin  in Asterias rubens.
The A. aranciacus population studied herein seems to have variable reproductive and recruitment success. Sea stars as other echinoderms show usually a high degree of spatial and temporal variability in settlement and recruitment . Nil or low recruitment over a period of time is not surprising in A. aranciacus, i.e., Hörstadius  reported that they have a long pelagic larval phase (80 days) under laboratory conditions. During this period Astropecten larvae were subject to hydrological processes which may displace them long distances [15, 41]. Regarding the main hydrological process in the study area, the prevailing currents are controlled by the cyclonic eddy of the western Mediterranean derived from the Liguro–Provencal current . Although local larvae could be transported away to the southwest, recruitment was already observed 2 of the 3 years studied on the nearshore area, indicating that some larvae settled. The lack of recruitment offshore may be related to the absence of favorable environmental conditions for larvae settlement and/or to predation on juveniles. During different samplings, offshore, we observed the presence of Luidia ciliaris and Tethyaster subermis, potential predators  that could play an important role in the recruitment failure of A. aranciacus.
Results showed that both A. aranciacus sexes had a synchronous gametogenesis but females reached the maturity stage slightly earlier than males, in accordance with previous results obtained in Asterias amurensis by Byrne et al. . The studied A. aranciacus population did not differ significantly in the male–female proportions, coinciding with previous results in other sexually reproducing asteroids (since sex-ratios can be highly biased in the case of asexual asteroids) [4, 26]. The development of the A. aranciacus gonads reflected that mature and partially spawned individuals remained for an extended period of time. The GI value was highest in March, indicating that during that month the gonads of A. aranciacus were in maximum development. Spawning likely started in March in part of the population and extended until June–July, in accordance with the decrease in GI and the presence of post-spawning individuals evidenced by the histological analysis of the gonads.
In general the reproductive cycles of sea stars are correlated with a combination of endogenous (i.e., hormones) and exogenous factors (i.e., temperature, photoperiod, food availability, lunar cycle, tidal flux and light intensity) . Sea star oocytes at the peak of the breeding season are fully grown and arrested at prophase I of meiosis . Hormonal stimulation (methyladenine, 1-MA) from the adhering follicle cells reenter the oocytes in the meiotic cycle before being spawned into seawater . However, the direct influence of exogenous factors remains still poorly understood . In Astropecten species, breeding season commonly coincides with the increase in water temperatures in temperate areas . For instance, these authors reported that the spawning periods for A. irregularis coincided with the rise from 8 to 15 °C in seawater temperatures (North Wales). Our results showed a similar pattern, because the spawning season of A. aranciacus likely began in spring, when the sea water temperatures started to increase in the Mediterranean. We also observed that the beginning of A. aranciacus spawning coincided with the highest Chl a concentration in the sea water, which was caused by the spring phytoplankton bloom typical of the Mediterranean Sea. The coincidence between the highest phytoplankton concentration and the spawning has been previously described in other echinoderms, but it is rare in sea stars . The majority of the species of the genus Astropecten have planktonic larvae (bipinnaria). Bipinnaria larva nourish essentially on detritus, bacteria, phytoplankton (mainly small diatoms and small flagellates) and small zooplankton . The synchronism between the spawning season of A. aranciacus, and the phytoplankton bloom could be a strategy to guarantee higher survival of early developmental stages.
An inverse correlation between GI and PCI has usually been described in most sea stars, suggesting the transfer of nutrients from the pyloric caeca to the gonads during gametogenesis . However, this interaction has not been observed in species inhabiting areas with stable environmental conditions . This relationship was not observed in the studied A. aranciacus population despite the fact that it inhabits a seasonally changing environment, in accordance with the results obtained by Ventura et al.  in A. cingulatus. Individuals of A. aranciacus collected in the offshore zone of the study area had large amount of preys in the stomach throughout the year. Most of these prey items were the venerid Timoclea ovata (>55 %, abundance in 224 sea stars analyzed), and each sea star stomach contains a mean of 49 T. ovata items of a mean size of 5.77 mm (SD = 5.52, N = 9682) . Therefore, food does not seem to be a limiting factor in the Maresme coast, suggesting that sea stars do not need to store large amounts of nutrients in the pyloric cecum, because nutrients can be easily obtained from the environment throughout all year. This suggests for A. aranciacus an “income breeding” reproductive strategy rather than “capital breeding”, i.e., reproduction is financed using current energetic income and not from stored energetic capital. This strategy may explain why an inverse correlation between GI and PCI was not observed in this population.
Our findings provide a better understanding of the biology of A. aranciacus in the NW Mediterranean Sea and are also relevant for the future conservation of this sea star, since its populations seem to decrease in some places of the Mediterranean Sea.
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All co-authors carried out the adquisition, analysis and interpretation of data, drafting and critical revision of the Manuscript.
This study is part of the doctoral dissertation of MB. We are grateful to the fishermen ‘Confraria de Pescadors d’Arenys’, in particular the clam dredge fishermen (Miguel Angel Ruiz Navas, Jose Luís López Ramírez, Mauricio Pulido and their sailors), and Jaume Germà from the bottom trawl fleet. We are also grateful to all sampling participants: Lucía Martínez, Marta Coca, Eduard Albella and Nil García. We deeply thank Anabel Colmenero for her advice and tips on histology techniques and for her constructive comments and suggestions on reproductive biology. We are very grateful to Dr. Francesc Peters for providing us with the chlorophyll data. The authors also thank Puertos del Estado (Instituto Geográfico Nacional, Ministerio de Fomento) for the environmental data and Raquel Ubach (Autonomous University of Barcelona) for the help with the map.
The authors declare that they do not have competing interests.
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Baeta, M., Galimany, E. & Ramón, M. Growth and reproductive biology of the sea star Astropecten aranciacus (Echinodermata, Asteroidea) on the continental shelf of the Catalan Sea (northwestern Mediterranean). Helgol Mar Res 70, 1 (2016). https://doi.org/10.1186/s10152-016-0453-z
- Mediterranean and echinoderm