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Pengabdian ini bertujuan mengembangkan kemampuan guru dalam menyusun instrumen penilaian berbasis Literasi dan Numerasi (Litnum) melalui pendampingan. Latar belakang pengabdian ini adalah kebutuhan mendesak untuk meningkatkan kualitas penilaian di sekolah-sekolah, mengingat pentingnya instrumen penilaian yang akurat untuk mengukur literasi dan numerasi siswa. Pendampingan dilakukan dalam tiga tahapan utama: 1) Pra Pendampingan, mencakup persiapan dan penyiapan materi; 2) Pendampingan, meliputi penyajian materi, diskusi kelompok, praktik penyusunan instrumen, dan presentasi; serta 3) Pasca Pendampingan, yang melibatkan pendalaman dan review. Hasil pengabdian menunjukkan bahwa pendampingan efektif meningkatkan kompetensi guru dalam menyusun instrumen penilaian berbasis Litnum dengan lima indikator keberhasilan: penyusunan kisi-kisi, stimulus soal, relevansi indikator, pedoman penskoran, dan rubrik penilaian. Capaian di atas 50% dinilai efektif karena peserta belum pernah mengikuti pendampingan serupa sebelumnya.

The COVID-19 pandemic changed many aspects of life, including learning process. Distance learning has been implemented as a response to the pandemic. These changes have a psychological impact on students. This study aims to explore the role of gratitude as a mediator in the relationship between social support and resiliency among students during distance learning. This study used quantitative method to 42 students (M=21,5). The study found that, while gratitude is not meaningful mediating variabel accounting for the relationship between social support and resilience, perceived social support predicts higher levels of resilience and gratitude among students participating in distance learning. While few participants reported that they adjusted well with the shift of learning mode, common challenges faced by participants which necessitates resilience in distance learning include: less enthusiasm in learning due to limited social interaction, poor time management, and exhaustion due to prolong exposure to screen.

Central Sulawesi is a part of Indonesia with a fascinating history during the revolutionary period (1945–1950), owing to several important events related to Indonesian sovereignty. This study uses historical methods to examine the involvement of the Netherlands Indies Civil Administration and its effort to recolonize the area. The Malino Conference, which led to the formation of the State of East Indonesia, was intended to legitimize the federated state under Dutch control and reduce the territory of the Republic of Indonesia. The Central Sulawesi Indonesian People’s Struggle Party is a unification of political parties that consistently maintained Central Sulawesi as part of the Republic of Indonesia, strengthening its bargaining position with the Dutch. This situation brought strong pressure to bear upon the Netherlands to immediately recognize the sovereignty of the Republic of Indonesia.

The current study aimed to see the correlation of perceived social support in enhancing resilience in international students towards academic stress and COVID-19 stress. Extend to which the coronavirus COVID-19 pandemic is affecting worldwide. This study explores social support and resilience towards academic stress and COVID-19 stress in international students—the sample of 83 International Asian and African students, respectively taken from different Countries and universities. The results revealed a significant effect of perceived social support and resilience towards COVID-19 stress. However, further results showed there was a non-significant relationship between perceived social support, resilience towards academic stress.

Prayer is a subjective experience that requires solemnity, by seeking a state of mindfulness and minimizing the state of mind wandering so that the prayer is done optimally. This study aims to explore the role of spirituality and religiosity to increase mindfulness and minimize mind-wandering in prayer activities, in Islamic preachers. Analysis was conducted through mixed method explanatory sequential analysis, using quantitative data with Multiple linear regression and qualitative data with Thematic analysis. Qualitative data (n = 3) was used to explore the experience of the meaning of mindfulness and mind-wandering conditions during prayer which was tested using quantitative data (n = 66). The quantitative analysis showed that mindfulness was negatively correlated with mind-wandering in prayer and that religious salience predicted mindfulness. Meanwhile, the experience of mind-wandering in prayer can be explained more qualitatively. There are 3 major themes regarding the experience of mindfulness and mind-wandering as well as the role of spirituality and religiosity in Islamic preachers, namely 1) solemn conditions, consisting of the involvement of a) mental representation, b) mental dialogue, c) expectation, d) control of consciousness, e) appreciation of life experience, and f) feeling comfortable and full of enjoyment, 2) mind-wandering distraction, which consists of the presence of a) worldly ambitions and b) perceptual distraction, and 3) spiritual atmosphere conditioning, consisting of a) preparation of prayer pillars, b) self-preparation, and c) asking for protection.

Using data from four deep fields (COSMOS, AEGIS, ECDFS, and CDFN), we studythe correlation between the position of galaxies in the star formation rate(SFR) versus stellar mass plane and local environment at $z10^{10.4-10.6}$ $M_{\odot}$), across all environments. At high redshift ($0.5

Abstract – This study aims to discover the experience of parents who lost their child as a result from political violence in 1998 and to outline their meaning-making process after the loss of their child. The study was conducted using qualitative method with phenomenological approach. Participants were parents of an undergraduate student who became the victim of the incident (some refer them as ‘Reformation Heroes’), approached through convenience sampling. Data were collected by using in-depth interviews. Several themes elicited from the interview results in both parents: sorrow and resentment; refusal of loss; loss of happiness, warmth, enthusiasm, and hope; detachment from social life; social support; justice effort; and faith. Analytical findings showed that eventhough the incident has occured more than 20 years ago, participants were still going through complicated grief. Parents construe their child’s death as an ongoing sacrifice effort for justice, hence they are commited to end it by demanding legal justice. Abstrak — Penelitian ini bertujuan untuk memahami pengalaman dan pemaknaan orang tua yang anaknya meninggal dalam peristiwa kekerasan politik pada tahun 1998. Penelitian dilakukan dengan metode kualitatif dan pendekatan fenomenologi. Partisipan merupakan orang tua dari mahasiswa yang menjadi korban pada peristiwa tersebut (sering disebut sebagai Pahlawan Reformasi) dan partisipan dipilih berdasarkan ketersediaan sumber daya peneliti. Pengambilan data dilakukan melalui proses wawancara mendalam. Dari hasil wawancara dengan partisipan, ditemukan beberapa tema dalam pengalaman dan pemaknaan ayah maupun ibu, yaitu kesedihan mendalam; kemarahan yang besar; tidak menerima kematian anak; kehilangan kebahagiaan, kehangatan, semangat, dan harapan; menarik diri dari kehidupan sosial; bangkit karena dukungan sosial; memperjuangkan keadilan hukum; serta keimanan. Hasil analisa menunjukkan bahwa meskipun sudah 20 tahun lebih berlalu sejak peristiwa kematian anak, partisipan masih terus mengalami perasaan berduka yang kompleks. Kedua orang tua memaknai kematian anak mereka sebagai pengorbanan dan perjuangan yang belum selesai. Oleh karena itu, mereka berkomitmen untuk menyelesaikan perjuangan tersebut dengan menuntut keadilan hukum.

We study the evolution of the total star formation (SF) activity, total stellar mass (∑M*) and halo occupation distribution (HOD) in massive haloes by using one of the largest X-ray selected sample of galaxy groups with secure spectroscopic identification in the major blank field surveys (ECDFS, CDFN, COSMOS, AEGIS). We provide an accurate measurement of star formation rate (SFR) for the bulk of the star-forming galaxies using very deep mid-infrared Spitzer MIPS and far-infrared Herschel PACS observations. For undetected IR sources, we provide a well-calibrated SFR from spectral energy distribution (SED) fitting. We observe a clear evolution in the level of SF activity in galaxy groups. The total SF activity in the high-redshift groups (0.5 < z < 1.1) is higher with respect to the low-redshift (0.15 < z < 0.5) sample at any mass by 0.8 ± 0.12 dex. A milder difference (0.35 ± 0.1 dex) is observed between the low-redshift bin and the groups at z ~ 0. We show that the level of SF activity is declining more rapidly in the more massive haloes than in the more common lower mass haloes. We do not observe any evolution in the HOD and total stellar mass-halo mass relations in groups. The picture emerging from our findings suggests that the galaxy population in the most massive systems is evolving faster than galaxies in lower mass haloes, consistently with a 'halo downsizing' scenario.

We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z ~ 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filamentlike' and field. Both methods show no evidence of an SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z ~ 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z ~ 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z ~ 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z ~ 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z ~ 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filamentlike' and field. Both methods show no evidence of an SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z ~ 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z ~ 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z ~ 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z ~ 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Body shaming, atau mempermalukan seseorang karena bentuk tubuhnya, baik yang dilakukan oleh diri sendiri maupun orang lain, dapat memicu respons negatif terhadap korban. Studi autoetnografi ini bertujuan untuk menggali bagaimana individu memaknai pengalaman malu terkait tubuh. Partisipan adalah peneliti sendiri dan dua orang wanita dewasa muda yang memiliki pengalaman malu terkait tubuh. Hasil studi ini menunjukkan bahwa pengalaman malu terkait tubuh memunculkan emosi negatif pada semua partisipan. Akan tetapi, terdapat dampak yang berbeda di setiap partisipan. Hasil studi dirangkum dalam tujuh tema besar, yaitu kemunculan malu terkait tubuh, alasan melakukan diet, dampak negatif, strategi koping, malu terkait tubuh saat dan setelah diet, dampak positif, dan dukungan menghadapi malu terkait tubuh. Penelitian ini diharapkan dapat meningkatkan pemahaman masyarakat tentang fenomena malu terkait tubuh, dampaknya, dan berbagai strategi untuk mengatasi pengalaman tersebut.

In the local Universe, galaxy properties show a strong dependence on environment. In cluster cores, early-type galaxies dominate, whereas star-forming galaxies are more and more common in the outskirts. At higher redshifts and in somewhat less dense environments (e.g. galaxy groups), the situation is less clear. One open issue is that of whether and how the star formation rate (SFR) of galaxies in groups depends on the distance from the centre of mass. To shed light on this topic, we have built a sample of X-ray selected galaxy groups at 0 < z < 1.6 in various blank fields [Extended Chandra Deep Field South (ECDFS), Cosmological Evolution Survey (COSMOS), Great Observatories Origin Deep Survey (GOODS)]. We use a sample of spectroscopically confirmed group members with stellar mass M* > 1010.3M* in order to have a high spectroscopic completeness. As we use only spectroscopic redshifts, our results are not affected by uncertainties due to projection effects. We use several SFR indicators to link the star formation (SF) activity to the galaxy environment. Taking advantage of the extremely deep mid-infrared Spitzer MIPS and far-infrared Herschel1 PACS observations, we have an accurate, broad-band measure of the SFR for the bulk of the star-forming galaxies. We use multi-wavelength Spectral Energy Distribution (SED) fitting techniques to estimate the stellar. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

In the local Universe, galaxy properties show a strong dependence on environment. In cluster cores, early-type galaxies dominate, whereas star-forming galaxies are more and more common in the outskirts. At higher redshifts and in somewhat less dense environments (e.g. galaxy groups), the situation is less clear. One open issue is that of whether and how the star formation rate (SFR) of galaxies in groups depends on the distance from the centre of mass. To shed light on this topic, we have built a sample of X-ray selected galaxy groups at 0 < z < 1.6 in various blank fields [Extended Chandra Deep Field South (ECDFS), Cosmological Evolution Survey (COSMOS), Great Observatories Origin Deep Survey (GOODS)]. We use a sample of spectroscopically confirmed group members with stellar mass M* > 1010.3M* in order to have a high spectroscopic completeness. As we use only spectroscopic redshifts, our results are not affected by uncertainties due to projection effects. We use several SFR indicators to link the star formation (SF) activity to the galaxy environment. Taking advantage of the extremely deep mid-infrared Spitzer MIPS and far-infrared Herschel1 PACS observations, we have an accurate, broad-band measure of the SFR for the bulk of the star-forming galaxies. We use multi-wavelength Spectral Energy Distribution (SED) fitting techniques to estimate the stellar. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Penelitian ini bertujuan untuk mengetahui pengalaman serta pemaknaan individu terhadap kematian kedua orang tua. Wawancara dengan desain fenomenologi dilakukan terhadap perempuan 23 tahun yang kehilangan kedua orang tua secara berurutan dalam waktu singkat. Data dianalisis menggunakan teknik deskripsi tekstural. Peristiwa meninggalnya ibu didahului dengan proses sakit yang panjang, sehingga muncul firasat buruk dan cemas. Sementara itu, kehilangan ayah yang mendadak memunculkan perasaan bingung dan penyangkalan. Setelah orang tua meninggal, partisipan merasa kosong dan sendirian, serta kehilangan motivasi dan arah. Setelah hampir empat tahun berlalu, marah kepada Tuhan dan kebingungan terhadap agama muncul bersama dengan konflik antar saudara. Secara keseluruhan, tema yang muncul adalah penyangkalan, depresi, dan kemarahan. Partisipan belum dapat menerima dan memaknainya sebagai peristiwa menyakitkan. Studi ini menggambarkan proses pemulihan yang tidak mudah pasca kehilangan yang berurutan, dan dukungan sosial yang tulus dan berkelanjutan, serta ruang untuk mengekspresikan emosi dibutuhkan untuk dapat mengatasi kedukaan secara adaptif.

Kleptomania merupakan sebuah gangguan yang dikarakteristikkan dengan adanya dorongan untuk melakukan tindakan mencuri benda-benda tidak dibutuhkan dan tidak menguntungkan. Dorongan tersebut muncul tak tertahankan dan terjadi berulang kali. Penelitian ini bertujuan untuk menggali bagaimana individu yang pernah menampilkan gejala kleptomania memaknai pengalaman terkait perilaku kleptomanianya. Untuk memahami fenomena tersebut dengan lebih mendalam, penelitian ini dilakukan dalam dua tahap, yaitu studi autoetnografi terhadap diri peneliti sendiri dan studi fenomenologi terhadap dua orang partisipan. Hasil kedua studi menunjukkan bahwa seluruh partisipan memunculkan perilaku kleptomania sejak usia anak-anak dan menunjukkan latar belakang keluarga yang tidak harmonis. Terdapat enam tema yang dimaknai secara berbeda antar partisipan, yaitu: kekecewaan kepada orang tua, perasaan putus asa, dorongan yang kuat, perasaan malu, perasaan tidak pernah puas, dan keinginan untuk memperbaiki diri. Enam tema tersebut kemudian disimpulkan menjadi tiga tema besar, yaitu: latar belakang keluarga, dinamika internal partisipan, dan keputusan untuk memperbaiki diri.

Penelitian ini bertujuan untuk memahami pengalaman dan pemaknaan orang tua yang anaknya meninggal dalam peristiwa kekerasan politik pada tahun 1998. Penelitian dilakukan dengan metode kualitatif dan pendekatan fenomenologi. Partisipan merupakan orang tua dari mahasiswa yang menjadi korban pada peristiwa tersebut (sering disebut sebagai Pahlawan Reformasi) dan partisipan dipilih berdasarkan ketersediaan sumber daya peneliti. Pengambilan data dilakukan melalui proses wawancara mendalam. Dari hasil wawancara dengan partisipan, ditemukan beberapa tema dalam pengalaman dan pemaknaan ayah maupun ibu, yaitu kesedihan mendalam; kemarahan yang besar; tidak menerima kematian anak; kehilangan kebahagiaan, kehangatan, semangat, dan harapan; menarik diri dari kehidupan sosial; bangkit karena dukungan sosial; memperjuangkan keadilan hukum; serta keimanan. Hasil analisa menunjukkan bahwa meskipun sudah 20 tahun lebih berlalu sejak peristiwa kematian anak, partisipan masih terus mengalami perasaan berduka yang kompleks. Kedua orang tua memaknai kematian anak mereka sebagai pengorbanan dan perjuangan yang belum selesai. Oleh karena itu, mereka berkomitmen untuk menyelesaikan perjuangan tersebut dengan menuntut keadilan hukum.

Author(s): R. Genzel (corresponding author) [1, 2]; N. M. Frster Schreiber (corresponding author) [1]; H. bler [1]; P. Lang [1]; T. Naab [3]; R. Bender [1, 4]; L. J. Tacconi [...]

Central Sulawesi is a part of Indonesia with a fascinating history during the revolutionary period (1945–1950), owing to several important events related to Indonesian sovereignty. This study uses historical methods to examine the involvement of the Netherlands Indies Civil Administration and its effort to recolonize the area. The Malino Conference, which led to the formation of the State of East Indonesia, was intended to legitimize the federated state under Dutch control and reduce the territory of the Republic of Indonesia. The Central Sulawesi Indonesian People's Struggle Party is a unification of political parties that consistently maintained Central Sulawesi as part of the Republic of Indonesia, strengthening its bargaining position with the Dutch. This situation brought strong pressure to bear upon the Netherlands to immediately recognize the sovereignty of the Republic of Indonesia. [ABSTRACT FROM AUTHOR]

A collaborative autoethnographic study was conducted to describe the authors’ experiences in an attempt to reconcile with Adverse Childhood Experiences (ACEs). The participants of this research are the author, together with her elder brother. Data were gathered from online personal diaries through blogger, digital journals, participants' memories and writings regarding ACEs, of which analyzed in the form of narrative themes. The result shows that changes could happen if a person reflects on themselves and find meanings through their experiences even though ACEs indeed had negative impacts in adulthood. Various meanings obtained through events written in autoethnography which then brings the author to the process of awareness, whilst enabling her to understand ACEs from different perspectives and build a new motivation to make efforts of overcoming the side effects of her past traumatic experiences. The research can provide insights for mental health professionals to help adults dealing with past trauma. Aside from that, autoethnography is part of therapeutic tools which are effective not just for the authors, but also the readers who faced the same struggles as the author, in this context, make peace with ACEs. This enhances the importance of doing the research, not only to benefit practitioners, but also for future readers who experienced ACEs itself. [ABSTRACT FROM AUTHOR]

We investigate what drives the redshift evolution of the typical electron density (ne) in star-forming galaxies, using a sample of 140 galaxies drawn primarily from KMOS3D (0.6 < z < 2.6) and 471 galaxies from SAMI (z < 0.113). We select galaxies that do not show evidence of active galactic nucleus activity or outflows to constrain the average conditions within H ii regions. Measurements of the [S ii ]λ6716/[S ii ]λ6731 ratio in four redshift bins indicate that the local ne in the line-emitting material decreases from 187 cm−3 at z ∼ 2.2 to 32 cm−3 at z ∼ 0, consistent with previous results. We use the Hα luminosity to estimate the rms ne averaged over the volumes of star-forming disks at each redshift. The local and volume-averaged ne evolve at similar rates, hinting that the volume filling factor of the line-emitting gas may be approximately constant across 0 ≲ z ≲ 2.6. The KMOS3D and SAMI galaxies follow a roughly monotonic trend between ne and star formation rate, but the KMOS3D galaxies have systematically higher ne than the SAMI galaxies at a fixed offset from the star-forming main sequence, suggesting a link between the ne evolution and the evolving main sequence normalization. We quantitatively test potential drivers of the density evolution and find that ne(rms) , suggesting that the elevated ne in high-z H ii regions could plausibly be the direct result of higher densities in the parent molecular clouds. There is also tentative evidence that ne could be influenced by the balance between stellar feedback, which drives the expansion of H ii regions, and the ambient pressure, which resists their expansion. [ABSTRACT FROM AUTHOR]

We present the brightest cluster galaxies (BCGs) catalog for SPectroscoic IDentification of eROSITA Sources (SPIDERS) DR14 cluster program value-added catalog. We list the 416 BCGs identified as part of this process, along with their stellar mass, star formation rates (SFRs), and morphological properties. We identified the BCGs based on the available spectroscopic data from SPIDERS and photometric data from SDSS. We computed stellar masses and SFRs of the BCGs on the basis of SDSS, WISE, and GALEX photometry using spectral energy distribution fitting. Morphological properties for all BCGs were derived by Sersic profile fitting using the software package SIGMA in different optical bands (g,r,i). We combined this catalog with the BCGs of galaxy groups and clusters extracted from the deeper AEGIS, CDFS, COSMOS, XMM-CFHTLS, and XMM-XXL surveys to study the stellar mass–halo mass relation using the largest sample of X-ray groups and clusters known to date. This result suggests that the mass growth of the central galaxy is controlled by the hierarchical mass growth of the host halo. We find a strong correlation between the stellar mass of BCGs and the mass of their host halos. This relation shows no evolution since z ∼ 0.65. We measure a mean scatter of 0.21 and 0.25 for the stellar mass of BCGs in a given halo mass at low (0.1 <  z <  0.3) and high (0.3 <  z <  0.65) redshifts, respectively. We further demonstrate that the BCG mass is covariant with the richness of the host halos in the very X-ray luminous systems. We also find evidence that part of the scatter between X-ray luminosity and richness can be reduced by considering stellar mass as an additional variable. [ABSTRACT FROM AUTHOR]

Context. The most striking feature of the cosmic star formation history (CSFH) of the Universe is a dramatic drop in the star formation (SF) activity after z ∼ 1. Aims. In this work we investigate whether the very same process of assembly and growth of structures is one of the major drivers of the observed decline in the Universe's SF activity. Methods. We study the contribution to the CSFH of galaxies in halos of different masses. This is done by studying the total SF ratehalo mass-redshift plane from redshift 0 to redshift ∼1.6 in a sample of 57 groups and clusters by using the deepest available midand far-infrared surveys conducted with Spitzer MIPS and Herschel PACS and SPIRE, on blank (ECDFS, CDFN, and the COSMOS) and cluster fields. Results. Our results show that low mass groups (Mhalo ∼ 6 × 1012-6 × 1013 M☉) provide a 60-80% contribution to the CSFH at z ∼ 1. This contribution has declined faster than the CSFH in the past 8 billion years to less than 10% at z < 0.3, where the overall SF activity is sustained by lower mass halos. More massive systems (Mhalo > 6 × 1013 M☉) provide only a marginal contribution (<10%) at any epoch. A simplified abundance-matching method shows that the large contribution of low mass groups at z ∼ 1 is due to a large fraction (>50%) of very massive, highly star-forming main sequence galaxies. Below z ∼ 1 a quenching process must take place in massive halos to cause the observed faster suppression of their SF activity. Such a process must be a slow one, though, since most of the models implementing a rapid quenching of the SF activity in accreting satellites significantly underpredict the observed SF level in massive halos at any redshift. This would rule out short time-scale mechanisms such as ram pressure stripping. Instead, starvation or the satellite's transition from cold to hot accretion would provide a quenching timescale of 1 to few Gyr that is more consistent with the observations. Conclusions. Our results suggest a scenario in which, owing to the structure formation process, more and more galaxies experience the group environment and the associated quenching process in the past 8 billion years. This leads to the progressive suppression of their SF activity so that it shapes the CSFH below z ∼ 1. [ABSTRACT FROM AUTHOR]

Context. There is now a large consensus that the current epoch of the cosmic star formation history (CSFH) is dominated by low mass galaxies while the most active phase, between redshifts 1 and 2, is dominated by more massive galaxies, which evolve more quickly. Aims. Massive galaxies tend to inhabit very massive haloes, such as galaxy groups and clusters. We aim to understand whether the observed "galaxy downsizing" could be interpreted as a "halo downsizing", whereas the most massive haloes, and their galaxy populations, evolve more rapidly than the haloes with lower mass. Methods. We studied the contribution to the CSFH of galaxies inhabiting group-sized haloes. This is done through the study of the evolution of the infra-red (IR) luminosity function of group galaxies from redshift 0 to redshift ~1.6. We used a sample of 39 X-rayselected groups in the Extended Chandra Deep Field South (ECDFS), the Chandra Deep Field North (CDFN), and the COSMOS field, where the deepest available mid- and far-IR surveys have been conducted with Spitzer MIPS and with the Photodetector Array Camera and Spectrometer (PACS) on board the Herschel satellite. Results. Groups at low redshift lack the brightest, rarest, and most star forming IR-emitting galaxies observed in the field. Their IR-emitting galaxies contribute ≤10% of the comoving volume density of the whole IR galaxy population in the local Universe. At redshift ≳1, the most IR-luminous galaxies (LIRGs and ULIRGs) are mainly located in groups, and this is consistent with a reversal of the star formation rate (SFR) vs. density anti-correlation observed in the nearby Universe. At these redshifts, group galaxies contribute 60-80% of the CSFH, i.e. much more than at lower redshifts. Below z ~ 1, the comoving number and SFR densities of IR-emitting galaxies in groups decline significantly faster than those of all IR-emitting galaxies. Conclusions. Our results are consistent with a "halo downsizing" scenario and highlight the significant role of "environment" quenching in shaping the CSFH. [ABSTRACT FROM AUTHOR]

A well-calibrated method to describe the environment of galaxies at all redshifts is essential for the study of structure formation. Such a calibration should include well-understood correlations with halo mass, and the possibility to identify galaxies which dominate their potential well (centrals), and their satellites. Focusing on z ~ 1 and 2, we propose a method of environmental calibration which can be applied to the next generation of low- to medium-resolution spectroscopic surveys. Using an up-to-date semi-analytic model of galaxy formation, we measure the local density of galaxies in fixed apertures on different scales. There is a clear correlation of density with halo mass for satellite galaxies, while a significant population of low-mass centrals is found at high densities in the neighbourhood of massive haloes. In this case, the density simply traces the mass of the most massive halo within the aperture. To identify central and satellite galaxies, we apply an observationally motivated stellar mass rank method which is both highly pure and complete, especially in the more massive haloes where such a division is most meaningful. Finally, we examine a test case for the recovery of environmental trends: the passive fraction of galaxies and its dependence on stellar and halo mass for centrals and satellites. With careful calibration, observationally defined quantities do a good job of recovering known trends in the model. This result stands even with reduced redshift accuracy, provided the sample is deep enough to preserve a wide dynamic range of density. [ABSTRACT FROM AUTHOR]

KMOS is a cryogenic infrared spectrograph fed by twentyfour deployable integral field units that patrol a 7.2 arcminute diameter field of view at the Nasmyth focus of the ESO VLT. It is well suited to the study of galaxy clusters at 1 < z < 2 where the well understood features in the restframe V-band are shifted into the KMOS spectral bands. Coupled with HST imagining, KMOS offers a window on the critical epoch for galaxy evolution, 7-10 Gyrs ago, when the key properties of cluster galaxies were established. We aim to investigate the size, mass, morphology and star formation history of galaxies in the clusters. Here we describe the instrument, discuss the status of the observations and report some preliminary results. [ABSTRACT FROM PUBLISHER]

The Pan-STARRS1 survey is obtaining multi-epoch imaging in five bands (gP1 rP1 IP1 zP1 yP1 ) over the entire sky north of declination - 30 deg. We describe here the implementation of the Photometric Classification Server (PCS) for Pan- STARRS1. PCS will allow the automatic classification of objects into star/galaxy/quasar classes based on colors and the measurement of photometric redshifts for extragalactic objects, and will constrain stellar parameters for stellar objects, working at the catalog level. We present tests of the system based on high signal-to-noise photometry derived from the Medium-Deep Fields of Pan-STARRS1, using available spectroscopic surveys as training and/or verification sets. We show that the Pan-STARRS1 photometry delivers classifications and photometric redshifts as good as the Sloan Digital Sky Survey (SDSS) photometry to the same magnitude limits. In particular, our preliminary results, based on this relatively limited data set down to the SDSS spectroscopic limits, and therefore potentially improvable, show that stars are correctly classified as such in 85% of cases, galaxies in 97%, and QSOs in 84%. False positives are less than 1% for galaxies, ≈19% for stars, and ≈28% for QSOs. Moreover, photometric redshifts for 1000 luminous red galaxies up to redshift 0.5 are determined to 2.4% precision (defined as 1.48 x Median zphot - zspec|/(1 + z)) with just 0.4% catastrophic outliers and small (-0.5%) residual bias. For bluer galaxies up to the same redshift, the residual bias (on average -0.5%) trend, percentage of catastrophic failures (1.2%), and precision (4.2%) are higher, but still interestingly small for many science applications. Good photometric redshifts (to 5%) can be obtained for at most 60% of the QSOs of the sample. PCS will create a value-added catalog with classifications and photometric redshifts for eventually many millions of sources. [ABSTRACT FROM AUTHOR]

ABSTRACT We have used the Visible Multi-Object Spectrograph (VIMOS) integral field spectrograph to map the emission-line properties in a sample of 24 star-forming galaxies selected from the Sloan Digital Sky Survey (SDSS) data base. In this paper we present and describe the sample, and explore some basic properties of SDSS galaxies with resolved emission-line fields. We fit the Hα+[N ii] emission lines in each spectrum to derive maps of continuum, Hα flux, velocity and velocity dispersion. The Hα, Hβ, [N ii] and [O iii] emission lines are also fit in summed spectra for circular annuli of increasing radius. A simple mass model is used to estimate dynamical mass within 10 kpc, which compared to estimates of stellar mass shows that between 10 and 100 per cent of total mass is in stars. We present plots showing the radial behaviour of equivalent width (EW)[Hα], u− i colour and emission-line ratios. Although EW[Hα] and u− i colour trace current or recent star formation, the radial profiles are often quite different. Whilst line ratios do vary with annular radius, radial gradients in galaxies with central line ratios typical of active galactic nucleus (AGN) or low-ionization nuclear emission-line regions are mild, with a hard component of ionization required out to large radii. We use our VIMOS maps to quantify the fraction of Hα emission contained within the SDSS fibre, taking the ratio of total Hα flux to that of a simulated SDSS fibre. A comparison of the flux ratios to colour-based SDSS extrapolations shows a 175 per cent dispersion in the ratio of estimated to actual corrections in normal star-forming galaxies, with larger errors in galaxies containing AGN. We find a strong correlation between indicators of nuclear activity: galaxies with AGN-like line ratios and/or radio emission frequently show enhanced dispersion peaks in their cores, requiring non-thermal sources of heating. Altogether, about half of the galaxies in our sample show no evidence for nuclear activity or non-thermal heating. The fully reduced data cubes and the maps with the line-fit results are available as FITS files from the authors. [ABSTRACT FROM AUTHOR]

Galaxy star formation rates (SFRs) are sensitive to the local environment; for example, the high-density regions at the cores of dense clusters are known to suppress star formation. It has been suggested that galaxy transformation occurs largely in groups, which are the intermediate step in density between field and cluster environments. In this paper, we use deep MIPS 24 µm observations of intermediate-redshift (0.3 ≲ z ≲ 0.55) group and field galaxies from the Group Environment and Evolution Collaboration (GEEC) subset of the Second Canadian Network for Observational Cosmology (CNOC2) survey to probe the moderate-density environment of groups, wherein the majority of galaxies are found. The completeness limit of our study is log(LTIR(L⊙)) ≳ 10.5, corresponding to SFR ≳2.7 M⊙ yr-1. We find that the group and field galaxies have different distributions of morphologies and mass. However, individual group galaxies have star-forming properties comparable to those of field galaxies of similar mass and morphology; that is, the group environment does not appear to modify the properties of these galaxies directly. There is a relatively large number of massive early-type group spirals, along with E/S0 galaxies, that are forming stars above our detection limit. These galaxies account for the nearly comparable level of star-forming activity in groups as compared with the field, despite the differences in mass and morphology distributions between the two environments. The distribution of specific SFRs (SFR/M*) is shifted to lower values in the groups, reflecting the fact that groups contain a higher proportion of massive and less active galaxies. Considering the distributions of morphology, mass, and SFR, the group members appear to lie between field and cluster galaxies in overall properties. [ABSTRACT FROM AUTHOR]

We present a multiscale approach for measurements of galaxy density, applied to a volume-limited sample constructed from the Sloan Digital Sky Survey Data Release 5 (SDSS DR5). We populate a rich parameter space by obtaining independent measurements of density on different scales for each galaxy. This parametrization purely relies on observations and avoids the implicit assumptions involved, e.g. in the construction of group catalogues. As the first application of this method, we study how the bimodality in galaxy colour distribution (specifically ) depends on multiscale density. The galaxy colour distribution is described as the sum of two Gaussians (a red and a blue one) with five parameters: the fraction of red galaxies ( fred) and the position and width of the red and blue peaks ( and σblue). Galaxies mostly react to their smallest scale ( ) environments: in denser environments red galaxies are more common (larger fred), redder (larger ) and with a narrower distribution (smaller σred), while blue galaxies are redder (larger ) but with a broader distribution (larger σblue). There are residual correlations of fred and with scale density, which imply that total or partial truncation of star formation can relate to a galaxy's environment on these scales. Beyond for ) there are no positive correlations with density. However fred anticorrelates with density on scales at fixed density on smaller scales, and anticorrelates with density on scales. We examine these trends qualitatively in the context of the halo model, utilizing the properties of haloes within which the galaxies are embedded, derived by Yang et al. and applied to a group catalogue. This yields an excellent description of the trends with multiscale density, including the anticorrelations on large scales, which map the region of accretion on to massive haloes. Thus we conclude that galaxies become red only once they have been accreted on to haloes of a certain mass. The mean colour of red galaxies depends positively only on scale density, which can most easily be explained if correlations of with environment are driven by metallicity via the enrichment history of a galaxy within its subhalo, during its epoch of star formation. [ABSTRACT FROM AUTHOR]

We have used the VIMOS Integral Field Unit to map the properties of the Seyfert 1.9 galaxy LEDA 135736. These maps reveal a number of interesting features including: an extended narrow-line region (ENLR) detectable out to ∼9 kpc, an area of intense star formation located at a projected distance of 12 kpc from the centre, an elliptical companion galaxy, and kinematic features, aligned along the long axis of the ENLR, that are consistent with radio jet driven mass outflow. We propose that the ENLR results from extraplanar gas ionized by the active galactic nucleus (AGN), and that the AGN in turn might be triggered by interaction with the companion galaxy, which can also explain the burst of star formation and morphological features. Only about 2 per cent of the ENLR's kinetic energy is in the mass outflow. We infer from this that the bulk of mechanical energy imparted by the jet is used to heat this gas. [ABSTRACT FROM AUTHOR]

The evolution of galaxies in groups may have important implications for the evolution of the star formation history of the Universe, since many processes which operate in groups may suppress star formation and the fraction of galaxies in bound groups grows rapidly betweenand the present day. In this paper, we present an investigation of the properties of galaxies in galaxy groups at intermediate redshift. The groups were selected from the Canadian Network for Observational Cosmology Redshift Survey (CNOC2) redshift survey as described by Carlberg et al., with further spectroscopic follow-up undertaken at the Magellan telescope in order to improve the completeness and depth of the sample. We present the data for the individual groups, and find no clear trend in the fraction of passive galaxies with group velocity dispersion and group concentration. We stack the galaxy groups in order to compare the properties of group galaxies with those of field galaxies at the same redshift. The groups contain a larger fraction of passive galaxies than the field, this trend being particularly clear for galaxies brighter thanin the higher velocity dispersion groups. In addition, we see evidence for an excess of bright passive galaxies in the groups relative to the field. In contrast, the luminosity functions of the star-forming galaxies in the groups and the field are consistent. These trends are qualitatively consistent with the differences between group and field galaxies seen in the local Universe. [ABSTRACT FROM AUTHOR]

We compare deep Magellan spectroscopy of 26 groups at, selected from the Canadian Network for Observational Cosmology 2 field survey, with a large sample of nearby groups from the 2PIGG catalogue. We find that the fraction of group galaxies with significant[O ii]λ3727 emission (≥5Å) increases strongly with redshift, from∼29 per cent in 2dFGRS to∼58 per cent in CNOC2, for all galaxies brighter than. This trend is parallel to the evolution of field galaxies, where the equivalent fraction of emission-line galaxies increases from∼53 to∼75 per cent. The fraction of emission-line galaxies in groups is lower than in the field, across the full redshift range, indicating that the history of star formation in groups is influenced by their environment. We show that the evolution required to explain the data is inconsistent with a quiescent model of galaxy evolution; instead, discrete events in which galaxies cease forming stars (truncation events) are required. We constrain the probability of truncation (Ptrunc) and find that a high value is required in a simple evolutionary scenario neglecting galaxy mergers. However, without assuming significant density evolution,Ptrunc is not required to be larger in groups than in the field, suggesting that the environmental dependence of star formation was embedded at redshifts. [ABSTRACT FROM AUTHOR]

In order to make informed decisions about the timing of harvests of grass crops, it is helpful to be aware of the changes that are taking place in the crops as they grow. Most people growing grass commercially or experimentally have a general awareness of the more obvious changes. However, greater awareness and understanding should lead to greater precision and greater success in the relevant enterprises. The present review considers some of the more important changes that are of interest from an agricultural point of view and for which sufficient information is available in the scientific literature. It is intended for relevant students, lecturers, research workers, advisers and producers. [ABSTRACT FROM PUBLISHER]

The purpose of this study was to investigate the effect of the stay-green trait, originally introduced into perennial ryegrass (Lolium perenne) for amenity purposes, in field swards of stay-green forage perennial ryegrass managed in different ways for agricultural use. The experimental treatments comprised all 18 combinations of two grass selections (stay-green and non-stay-green), three intervals between cuts and three N treatments. The conclusions were that the introduction of the stay-green trait (1) may not always confer greater greenness in the early life of a sward; (2) may confer greater greenness during leaf senescence more because carotenoids are unmasked to a lesser extent than because of a reduction in the length of leaf visibly senescing; (3) may reduce herbage yield, particularly when a long interval is allowed between defoliations; (4) may reduce the decline in the concentration of N in herbage during the latter part of a long period of regrowth; (5) may reduce the concentration of Na in herbage. [ABSTRACT FROM AUTHOR]

Investigates the relationships among education, liberal sex-role values, gender-role orientation, career commitment and employment level for a sample of married Indonesian women. Liberal sex-role values and masculinity as significant predictors of career commitment; Prediction of employment level through education.

In a field experiment with Italian ryegrass residual effects of N applied in late April at four rates, 28, 84, 140 and 196 kg ha-1, and of different dates of first harvest ranging from 1 to 14 weeks after N application, were studied. The harvests after the first added about 10 kg dry matter yield and about 0.16 kg N yield for each extra kg N applied in April. Residual response was similar for each increment of applied N. A positive residual response to N was obtained in May of the year following N application despite high winter rainfall. N content of herbage during part of the summer was reduced by extra N applied in April although N yield was increased. The reduction in N content was accompanied by a reduction in P and K content, these latter elements having been applied only once and at a uniform rate on all plots. Loss of N, P and K from the crop, when a period of more than about 9 weeks regrowth was allowed prior to the first harvest, was not recouped at subsequent harvests. Residual marginal recovery of N in Aberystwyth was no higher than in comparable experiments in Cambridge although marginal recovery of N at the first harvest had been appreciably lower in Aberystwyth than in Cambridge. [ABSTRACT FROM AUTHOR]

The regrowth of Italian ryegrass was studied at weekly intervals from 2 to 14 weeks after a cut in late April when 140 kg ha-¹ N was applied. Reduction in digestibility with delay in date of harvest was due to both an increase in the proportion of cell wall and a reduction in the digestibility of the cell wall, particularly the former from week 2 to about week 5 and particularly the latter after week 5. The reduction in the digestibility of the cell wall was about equally attributable to reduction in digestibility of cellulose and to reduction in digestibility of hemicellulose. The proportion of lignin in cell wall was highly correlated with both digestibility of cellulose and digestibility of hemicellulose. The proportion of digestible cell wall in dry matter was not as constant as has sometimes been noted, increasing by about 5 percentage units from week 2 to week 5 and decreasing by about 10 percentage units from week 5 to week 13. During the latter period the decline in digestible cell wall in dry matter accounted for nearly half the decline in true digestibility of dry matter. The ratio of cellulose: hemicellulose averaged 1:0.89 and hemicellulose was more digestible than cellulose. Rate of increase in yield of cell contents appeared to diminish from about the third week of regrowth onwards, whereas the rate of increase in yield of dry matter did not begin to diminish until about the seventh week. In vitro dry matter digestibility was not increased by adding extra N to the digestion tubes, even with samples containing only 1% N in dry matter. [ABSTRACT FROM AUTHOR]

Perennial ryegrass was sown in a field trial with or without a small-leaved white clover, SI 84, in September 1969 and cut five times per year in 2 successive years. Yield of clover was low and very unevenly distributed in time. Clover performance is described in four distinct periods, April-June 1970, July-September 1970, April- June 1971 and July-September 1971, in which yield of clover was respectively low, moderate, low and fairly high and the indirect contribution, the enhanced yield of other sward components, was respectively nil, moderate, moderate and moderate. The ratio of indirect to direct contributions on an annual basis concealed very large differences both within and between years. The presence of clover increased the N content but did not affect the P or K content of other sward components. [ABSTRACT FROM AUTHOR]

Herbage at various stages of growth from three field experiments, one with Italian ryegrass, one with perennial ryegrass and one with white clover, red clover and lucerne, was incubated for 0, 24 or 48 h in rumen liquor followed by 48 h in acid-pepsin. The proportion of cell content OM in herbage (measured by pepsin) declined with advancing stage of growth more quickly in the legumes than in Italian ryegrass. At a high level of digestibility the legumes had a higher proportion of cell content OM than Italian ryegrass, but the position tended to be reversed at a low level of digestibility. Decline in proportion of cell content and decline in digestibility of cell wall were both major contributors to the decline in digestibility of Italian ryegrass with advancing maturity, whereas in white clover the decline in proportion of cell content was entirely responsible for the decline in digestibility. Lucerne and red clover occupied intermediate positions. At an early vegetative stage rate of digestion appeared to be higher in Italian than in perennial ryegrass. Rate of digestion was higher in the legumes than in the ryegrasses, the difference being largest at an advanced stage of growth. [ABSTRACT FROM AUTHOR]

The regrowth of Italian ryegrass following a cut in late April was studied at weekly intervals up to 14 weeks. There were four levels of applied N: 28, 84, 140 and 196 kg ha-¹. The proportion of green leaf blade declined from 80% of DM yield after 2 or 3 weeks of regrowth to 5% after 13–14 weeks. About three-quarters of the increase in DM yield of total herbage from week 3 to week 11 was attributable to increased yield of ‘stem’. The level of applied N had little effect on the proportion of crop fractions except during the period immediately before and after the beginning of ear emergence when the higher rates of N increased the proportion of ‘stem’ and reduced that of green leaf. The most digestible crop fractions were green leaf, inflorescence and immature ‘stem’. D-value of ‘stem’ declined by about 20 units from week 1 to week 14, while D-value of green and dead leaf declined at about half this rate and there was little or no decline in D-value of inflorescence. The N content of green leaf was consistently higher than that of the other fractions. The N content of 'stem' declined markedly to around 0.5% by week 12. The N content of dead leaf and inflorescence was intermediate between that of green leaf and mature ‘stem’. The N content of all fractions was increased by applying more N. The tiller population increased during the first 3 weeks of regrowth and declined during the next 4. Applying more N increased both tiller population and weight per tiller. [ABSTRACT FROM AUTHOR]

In an experiment, described earlier (19) to study the regrowth of Italian ryegrass following a cut in late April, the N and nitrate-N content of herbage at 3 levels of applied N followed a similar pattern to that noted in earlier years in Cambridge. N content, however, did not faIl to such a low level as in Cambridge. N yield fell later and less quickly than in Cambridge. The application of a very high level of N, 175 lb/ac (196 kg/ha), raised N and nitrate-N content and yield from the second or third week onwards. Changes with time in P and K content and yield were broadly similar to those for N. Level of N had only a small effect on content of P and K. Following the period of increase in yield of N, P and K, there was a period of about 6 weeks of relatively constant yield, followed by a fall. The content of N, P and K in fresh, rather than dry, herbage changed little with time from the fourth to the fourteenth week, despite major changes in crop maturity. The ratio P : K was little affected by level of N or time of harvest. [ABSTRACT FROM AUTHOR]

True dry matter digestibility, proportion of cell content, digestibility of cell wall, N and water-soluble carbohydrate were determined in eight related grasses in February, June and September in each of three years. In a separate experiment, true dry matter digestibility, proportion of cell content and digestibility of cell wall were determined in five plant parts of vegetative tillers of two grasses in February, April, June, August, October and December in each of two years.Perennial ryegrass (Lolium perenne) was the most digestible grass and tall fescue (Festuca arundinacea) and Westerwolds ryegrass (Lolium multiflorum var. Westerwoldicum) were the least digestible. Italian ryegrass (Lolium multiflorum) was high in proportion of cell content, but not in digestibility of cell wall. Meadow fescue (Festuca pratensis) was high in digestibility of cell wall, but low in proportion of cell content. Perennial ryegrass and hybrid ryegrass were high, and tall fescue low, in both proportion of cell content and digestibility of cell wall. Ryegrasses were lower than fescues in concentration of N and higher than the fescues in water-soluble carbohydrate; ryegrass × meadow fescue hybrids were intermediate between the parent species in N and watersoluble carbohydrate.Grass sampled in June and August was lower in both proportion of cell content and digestibility of cell wall than grass sampled at cooler times of year. Grass sampled in February was high in proportion of cell content and N, intermediate to high in digestibility of cell wall and intermediate in water-soluble carbohydrate.Expanding leaf blades of perennial and Italian ryegrass were higher than expanded blades and sheaths in digestibility of cell wall and similar to expanded blades and higher than sheaths in proportion of cell content. Cell wall was less digestible in the tip than in the middle and basal portions of expanded leaf blades. [ABSTRACT FROM PUBLISHER]