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Chronic conditions are common in childhood. We investigated the associations of childhood chronic conditions reported by parents with subsequent self-reported internalizing and externalizing problems in adolescence. A sample of 6290 children (3142 boys and 3148 girls) with data on chronic condition reported by parents both at 7 and at 16 years of age was obtained from the Northern Finland Birth Cohort 1986 (NFBC 1986), which is a longitudinal 1-year birth cohort (n = 9432) from an unselected, regionally defined population. Internalizing and externalizing problems were measured at 8 years of age with Rutter Children’s Behavioral Questionnaire by teachers and at 16 years of age with Youth Self-Report by adolescents. When studying the effects of history of chronic conditions on these problems at 16 years of age, childhood internalizing and externalizing problems and social relations were adjusted. A history of chronic condition predicted subsequent somatic complaints among all adolescents. Early-onset chronic conditions were related to subsequent externalizing (OR 1.35; 1.02–1.79) and attention problems (OR 1.33; 1.01–1.75) and later onset of chronic conditions with internalizing (OR 1.49; 1.22–1.82) and thought problems (OR 1.50; 1.18–1.92). The effect was specific for sex and the type of chronic condition. Conclusion: Childhood chronic conditions predicted internalizing and externalizing problems in adolescence. To prevent poor mental health trajectories, children with chronic conditions during their growth to adolescence need early support and long-term monitoring.

Harsh parenting can predispose a child to emotional distress, whereas a supportive childhood environment furthers later subjective well-being. We investigated whether the mother’s self-reported assessment of her strictness and the adult offspring’s recollections of the disciplinary methods of their parents are reflected in the adult offspring’s recalled parental images and current emotional distress, anxiety and depression as assessed by the Hopkins Symptom Check List (HSCL-25). Further, we investigated whether the offspring’s parental images were also associated with the HSCL-25 scores. Data was collected from northern Finland. The mothers responded to a questionnaire when their child was seven years old (N = 354) and the adult offspring responded at age 28–29 (N = 337). The mother’s assessment of her own strictness was associated both with the adult offspring’s dominating images of their parents and their current emotional distress, anxiety and depression. The offspring’s recollections of restriction and corporal punishment were associated with dominating parental images, and these images further with current emotional distress, anxiety and depression of the offspring. Correspondingly, the offspring’s recollections of parental dialogic discipline were associated with supportive and sociable parental images, and recalled paternal dialogic discipline was associated with lower current emotional distress, particularly in the female offspring. In conclusion, harsh parenting was associated with dominating parental images, which in turn were associated with emotional distress in adulthood. Dialogic discipline and the father’s role in parenting were emphasized in the offspring’s well-being, but more research is needed to assess the importance of paternity for the offspring’s subjective well-being.

The aim of this longitudinal study was to investigate early vocabulary development and its relationships with prelinguistic communication skills and social-emotional/behavioral (SEB) problems and competencies. The participants were 58 healthy Finnish-speaking children (30 girls, 28 boys). First, the concurrent relationships were investigated at the age of 18 months. Second, the relationships between prelinguistic communication skills and SEB problems and competencies at 18 months, and subsequent vocabulary scores at 24 and 30 months, were examined. Parental reports on early vocabulary (MacArthur Communicative Developmental Inventories; MCDI), prelinguistic communication skills (The Infant-Toddler Checklist of the Communication and Symbolic Behavior Scales Developmental Profile; ITC), SEB problems and competencies (Brief Infant-Toddler Social and Emotional Assessment; BITSEA) were gathered. Compared to boys, girls scored significantly higher on ITC Speech Composite at 18 months and expressive vocabulary measures at 18, 24, and 30 months. Vocabulary, as well as prelinguistic communication measures, correlated with SEB competencies at 18 months. Furthermore, vocabulary, as well as ITC Symbolic Composite and Total Score, correlated negatively with externalizing problem and SEB Total Problem scores. With regard to subsequent vocabulary development, all of the prelinguistic communication measures at 18 months correlated with vocabulary at 24 and 30 months. However, when accounted for gender and earlier vocabulary, only the associations with ITC Speech Composite and Total Score at 24 months remained significant. SEB Competencies at 18 months correlated positively, while externalizing problems at 18 months correlated negatively with vocabulary at 24 and 30 months, however, these associations did not remain significant, when accounted for gender and earlier vocabulary.

ti Autismikirjon piirteet ulottuvat sosiaalisten taitojen, kommunikaation, mielikuvituksen, tarkkaavuuden siirtämisen ja yksityiskohtien huomioimisen alueille. Näillä osa-alueilla esiintyviä piirteitä voidaan seuloa autismikirjon osamäärän (engl. autism spectrum quotient, AQ) avulla. Tämän tutkimuksen tavoitteena on saada suomalaiset viitearvot AQ:lle sekä tarkastella, erotteleeko AQ-lomake suomalaisia autismikirjon nuoria aikuisia oman sukupuolen nuorista aikuisista, joilla ei ole autismikirjon diagnoosia. Lisäksi tarkastellaan ryhmien suoriutumisessa olevia eroja osioittain sekä AQ:n sisäistä yhtenäisyyttä. Tutkimukseen osallistui 52 autismikirjon nuorta aikuista (39 miestä ja 13 naista) sekä 1686 verrokkia (577 miestä ja 1109 naista). Tulokset osoittavat, että autismikirjon henkilöiden pistemäärät nousevat samaa sukupuolta olevien verrokkihenkilöiden pistemääriä korkeammalle. AQ erottelee autismikirjon miehet melko hyvin verrokkimiehistä, mutta autismikirjon naiset vain kohtalaisesti verrokkinaisista. Osioanalyysissä eniten ryhmien välisiä tilastollisesti merkitseviä eroja tuli esille sosiaalisia taitoja ja kommunikaatiota mittaavissa väittämissä. Abstract Autism spectrum quotient (AQ) in screening features of autism spectrum : discriminatory ability of screening form in young adults Features of autism spectrum include areas of social skills, communication, imagination, attention switching and attention to details. These features can be screened with Autism Spectrum Quotient (AQ). The purpose of this study is to obtain Finnish performance values for AQ and to study whether the AQ discriminates Finnish young adults on the autism spectrum from same-gender controls without autism spectrum diagnosis. In addition, differences between groups in each item and internal consistency of AQ has been studied. A total of 52 young adults on the autism spectrum (39 males and 13 females) and 1686 controls (577 males and 1109 females) took part in this study. Results show that individuals on the autism spectrum have higher scores than same-gender controls. AQ discriminates quite well males on the autism spectrum from control males but only fairly females on the autism spectrum from control females. In item analysis most statistically significant differences between groups were found in items measuring social skills and communication.

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Objective: Adolescence is a vulnerable age for emerging mental health problems, but also a time at which the foundations for a healthy lifestyle are established. Attitudes towards mental health problems and the ability to recognise them can be affected at this age. The aim of this study was to describe a psychoeducative intervention aimed at increasing knowledge of mental health problems and decreasing the stigma of mental health disorders among eighth-grade students in Finland. Design: Mixed-methods exploration of how a universal psychoeducation delivered in the classroom can affect attitudes towards, and recognition of, mental health disorders and how young people perceive the psychoeducation received. Setting: The study involved 162 eighth-grade students in two comprehensive schools in Finland. Method: The intervention consisted of four lessons on the topics of anxiety, eating disorders, conduct disorder, and depression and substance use. Results: Students in both the intervention and non-intervention groups recognised the symptoms of mental health disorders well before and after the intervention, and the intervention improved boys’ ability to recognise conduct disorder. Following the intervention, students saw mental health disorders as real medical conditions. Students experienced the intervention as beneficial, increasing their knowledge, understanding and open-mindedness with regards to mental health. Conclusions: Mental health promotion interventions have the goal of increasing the ability of individuals to understand mental health issues and engage in self-care of mental health. Providing mental health promotion interventions to young people has the potential to increase knowledge and skills in maintaining a healthy lifestyle in adulthood.

Tiivistelmä Mielenterveyden häiriöiden synnyn ja hoidon kannalta lapsuuden tekee erityiseksi aivojen voimakas muovautuvuus. Muovautuvuuden vuoksi aivot ovat herkemmät kielteisten kokemusten vaikutuksille, mutta toisaalta hoidolla on mahdollista korjata vaurioita ja mahdollistaa myöhempi terve kehitys. Lasten mielenterveyden häiriöiden hoito koostuu monista hoito- ja kuntoutusmenetelmistä, joista psykoterapia on yksi. Tavallisimmat leikki- ja kouluikäisten lasten mielenterveyden häiriöiden hoitoon käytettävät psykoterapian muodot ovat kognitiivinen käyttäytymisterapia, psykodynaaminen psykoterapia ja perhepsykoterapia. Asianmukaisella psykoterapeuttisella hoidolla voidaan usein korjata lapsen mielenterveyden häiriöön liittyneitä haitallisia ajatus- ja käyttäytymismalleja, parantaa lapsen toimintakykyä kotona ja kodin ulkopuolella sekä mahdollistaa myöhempi iänmukainen kehitys. Varhain toteutettu hoito vähentää lasten ja perheiden inhimillistä kärsimystä, ehkäisee syrjäytymistä ja säästää terveydenhuollon voimavaroja. Abstract Child psychotherapy The plasticity of the brain makes childhood an important period for the development and treatment of mental health disorders. Due to this plasticity, adverse childhood experiences have a stronger effect on the developing brain. However, this same plasticity may also enhance the effects of treatment, making later healthy development possible. Psychotherapy is one method for treating mental health disorders in childhood. The most common types of child psychotherapy currently used in Finland are cognitive-behavioral psychotherapy, psychodynamic psychotherapy, and family psychotherapy. With adequate psychotherapeutic treatment, it is often possible to alter a child’s dysfunctional thought and behaviour patterns, help the child function better both within and outside the home, and enable later age-appropriate psychological development. The early treatment of children’s mental health problems reduces the suffering of the child and the family. Furthermore, it reduces the risk of exclusion from society, and thus saves social and health service resources in the long run.

Social and pragmatic difficulties in autism spectrum disorder (ASD) are widely recognized, although their underlying neural level processing is not well understood. The aim of this study was to examine the activity of the brain network components linked to social and pragmatic understanding in order to reveal whether complex socio-pragmatic events evoke differences in brain activity between the ASD and control groups. Nineteen young adults (mean age 23.6 years) with ASD and 19 controls (mean age 22.7 years) were recruited for the study. The stimulus data consisted of video clips showing complex social events that demanded processing of pragmatic communication. In the analysis, the functional magnetic resonance imaging signal responses of the selected brain network components linked to social and pragmatic information processing were compared. Although the processing of the young adults with ASD was similar to that of the control group during the majority of the social scenes, differences between the groups were found in the activity of the social brain network components when the participants were observing situations with concurrent verbal and non-verbal communication events. The results suggest that the ASD group had challenges in processing concurrent multimodal cues in complex pragmatic communication situations.

This study investigated whole‐brain dynamic lag pattern variations between neurotypical (NT) individuals and individuals with autism spectrum disorder (ASD) by applying a novel technique called dynamic lag analysis (DLA). The use of 3D magnetic resonance encephalography data with repetition time = 100 msec enables highly accurate analysis of the spread of activity between brain networks. Sixteen resting‐state networks (RSNs) with the highest spatial correlation between NT individuals (n = 20) and individuals with ASD (n = 20) were analyzed. The dynamic lag pattern variation between each RSN pair was investigated using DLA, which measures time lag variation between each RSN pair combination and statistically defines how these lag patterns are altered between ASD and NT groups. DLA analyses indicated that 10.8% of the 120 RSN pairs had statistically significant (P‐value

The symptoms of ADHD tend to have continuity to adulthood even though the diagnostic criteria were no longer fulfilled. The aim of our study was to find out possible differences in BOLD signal in the face-processing network between adults with previous ADHD (pADHD, n = 23) and controls (n = 29) from the same birth cohort when viewing dynamic facial expressions. The brain imaging was performed using a General Electric Signa 1.5 Tesla HDX. Dynamic facial expression stimuli included happy and fearful expressions. The pADHD group demonstrated elevated activity in the left parietal area during fearful facial expression. The Network Based Statistics including multiple areas demonstrated higher functional connectivity in attention related network during visual exposure to happy faces in the pADHD group. Conclusions: We found differences in brain responses to facial emotional expressions in individuals with previous ADHD compared to control group in a number of brain regions including areas linked to processing of facial emotional expressions and attention. This might indicate that although these individuals no longer fulfill the ADHD diagnosis, they exhibit overactive network properties affecting facial processing.

We quantify the star formation (SF) in the inner cores ($\mathcal{R}$/$R_{200}$$\leq$0.3) of 24 massive galaxy clusters at 0.2$\lesssim$$z$$\lesssim$0.9 observed by the $Herschel$ Lensing Survey and the Cluster Lensing and Supernova survey with $Hubble$. These programmes, covering the rest-frame ultraviolet to far-infrared regimes, allow us to accurately characterize stellar mass-limited ($\mathcal{M}_{*}$$>$$10^{10}$ $M_{\odot}$) samples of star-forming cluster members (not)-detected in the mid- and/or far-infrared. We release the catalogues with the photometry, photometric redshifts, and physical properties of these samples. We also quantify the SF displayed by comparable field samples from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We find that in intermediate-$z$ cluster cores, the SF activity is suppressed with respect the field in terms of both the fraction ($\mathcal{F}$) of star-forming galaxies (SFG) and the rate at which they form stars ($\mathcal{SFR}$ and $s\mathcal{SFR} = \mathcal{SFR}/\mathcal{M}_{*}$). On average, the $\mathcal{F}$ of SFGs is a factor $\sim$$2$ smaller in cluster cores than in the field. Furthermore, SFGs present average $\mathcal{SFR}$ and $s\mathcal{SFR}$ typically $\sim$0.3 dex smaller in the clusters than in the field along the whole redshift range probed. Our results favour long time-scale quenching physical processes as the main driver of SF suppression in the inner cores of clusters since $z$$\sim$0.9, with shorter time-scale processes being very likely responsible for a fraction of the missing SFG population., 34 pages, 13 figures, 15 tables; accepted for publication in MNRAS

Tiivistelmä Tausta: Kartoitimme kyselyn avulla, miten vanhemmat ovat kokeneet lapsensa autismikirjon häiriön varhaisen tunnistamisen ja diagnosointiprosessin. Aineisto ja menetelmät: Kysely perustui ASDEU (the Autism Spectrum Disorders in the Europan Union) ‑hankkeen yhteiseen kyselyyn, joka käännettiin suomeksi. Kaikkiaan 51 perhettä vastasi verkkokyselyyn. Tulokset: Autismikirjon häiriö tunnistettiin keskimäärin 1,9 vuoden iässä (vaihtelu 1,1–5,2) ja diagnoosi asetettiin 3,9 vuoden iässä (vaihtelu 1,3–6,9). Vanhemmat olivat tyytyväisiä työntekijöiden ammattitaitoon mutta toivoivat, että heidän huolensa olisi otettu vakavasti ja lapsi lähetetty jatkotutkimuksiin nopeammin. Diagnoosin asettamisen jälkeen vanhemmat toivoivat lääkäriltä enemmän aikaa keskusteluun. Päätelmät: Vanhempia on tärkeä kuunnella autismikirjon häiriön tunnistamisessa, ja neuvolaseulontaa on hyvä kehittää. Siten olisi mahdollista varhentaa lapsen diagnoosin saamista. Abstract Background: The aim was to screen how parents have experienced identification and diagnosing of autism spectrum disorder (ASD). Material and Methods: The survey was based on the ASDEU questionnaire, which was translated into the Finnish language. Altogether 51 families answered the web questionnaire. Results: ASD was identified at the age of 1.9 y (range 1.1–5.2) and the diagnosis set at 3.9 y (range 1.3–6.9). Parents were satisfied with the professionals’ skills, but wished that their concerns had been taken seriously and the children referred to further evaluations quickly. After setting the diagnosis, the parents wanted more time for discussion with a pediatrician. Conclusions: The time between the identification to diagnosis is still long in Finland. It is important to listen to the parents about the identification of autism, and it would be good to develop a screening of ASD in child health care centers.

This longitudinal study aimed at showing the effect of early social-emotional/behavioural problems and competencies on vocabulary development in toddlers. The participants were 60 native Finnish-speaking healthy children (30 boys and 30 girls). Parental reports on the Brief Infant-Toddler Social and Emotional Assessment (BITSEA) were gathered at the children’s age of 18 months. The Problem Total and Competence Total, as well as externalizing, internalizing and dysregulation problem domain, scores were calculated. Vocabulary development was assessed by a certified speech and language therapist at ages 24 and 30 months using the Receptive and Expressive One-Word Picture Vocabulary Tests (ROWPVT-4 and EOWPVT-4). Compared to boys, girls obtained higher Competence Total scores and scored considerably higher in all the vocabulary measures. With regard to the relationships between early social-emotional/behavioural problems and vocabulary measures, Problem Total scores correlated negatively with receptive vocabulary scores at 24 months and expressive vocabulary scores at 30 months. Further analyses indicated that particularly externalizing problems were associated with slower vocabulary development. By contrast, Competence Total scores correlated positively with expressive vocabulary at 30 months. The same analyses were carried out separately for boys and girls. Mostly, the separate findings were in line with the results for the whole group of children.

International audience; We report on the galaxy MACSJ0032‐arc at z(CO) = 3.6314 discovered during the Herschel Lensing snapshot Survey of massive galaxy clusters, and strongly lensed by the cluster MACSJ0032.1+1808. The successful detections of its rest‐frame ultraviolet (UV), optical, far‐infrared (FIR), millimeter, and radio continua, and of its CO emission enable us to characterize, for the first time at such a high redshift, the stellar, dust, and molecular gas properties of a compact star‐forming galaxy with a size smaller than 2.5 kpc, a fairly low stellar mass of 4.8(‐1.0)(+0.5) x 10(9) M circle dot, and a moderate IR luminosity of 4.8(‐0.6)(+1.2) x 10(11) L circle dot. By combining the stretching effect of the lens with the high angular resolution imaging of the CO(10) line emission and the radio continuum at 5 GHz, we find that the bulk of the molecular gas mass and star formation seems to be spatially decoupled from the rest‐frame UV emission. About 90% of the total star formation rate is undetected at rest‐frame UV wavelengths because of severe obscuration by dust, but is seen through the thermal FIR dust emission and the radio synchrotron radiation. The observed CO(43) and CO(65) lines demonstrate that high‐J transitions, at least up to J = 6, remain excited in this galaxy, whose CO spectral line energy distribution resembles that of high‐redshift submm galaxies, even though the IR luminosity of MACSJ0032‐arc is ten times lower. This high CO excitation is possibly due to the compactness of the galaxy. We find evidence that this high CO excitation has to be considered in the balance when estimating the CO‐to‐H‐2 conversion factor. Indeed, the respective CO‐to‐H‐2 conversion factors as derived from the correlation with metallicity and the FIR dust continuum can only be reconciled if excitation is accounted for. The inferred depletion time of the molecular gas in MACSJ0032‐arc supports the decrease in the gas depletion timescale of galaxies with redshift, although to a lesser degree than predicted by galaxy evolution models. Instead, the measured molecular gas fraction as high as 6079% in MACSJ0032‐arc favors the continued increase in the gas fraction of galaxies with redshift as expected, despite the plateau observed between z similar to 1.5 and z similar to 2.5.

(Abridged) We present a morphological analysis of 17 X-ray selected clusters at z~0.25, imaged uniformly with HST WFPC2. Eight of these clusters have low X-ray luminosities (10^{45} ergs/s. The clusters cover a relatively small range in redshift and the data are homogeneous in terms of depth, resolution and rest wavelength observed. We use GIM2D to fit the two dimensional surface brightness profiles of galaxies down to M(702), Astrophysical Journal, accepted (tent. Feb 10 2002, vol 566) 13 pages, emulateapj style with 9 in-line figures

Fraunhofer ICT was approached by TAKATA Corporation to assist in investigations on unintended energetic disassembly of airbag inflators. Fundamental investigations on the AN based pyrotechnic main propellant revealed no problem with typical failure modes of pyrotechnic propellant e.g. phase stabilization of AN or chemical stability. Morphological changes and generation of pores in the core of the propellant grain were identified leading to an increased burn rate by so called porous burning mechanism. Additional investigations focused on characterization of moisture intrusion into the inflator and replication of moisture intrusion by environmental simulation programs used for product validation.

Radio halos are synchrotron radio sources detected in some massive galaxy clusters. Their Mpc-size indicates that (re)acceleration processes are taking place in the host cluster. X-ray catalogues of galaxy clusters have been used in the past to search for radio halos and to understand their connection with cluster-cluster mergers and with the thermal component of the intra-cluster medium. More recently, the Sunyaev-Zel'dovich effect has been proven to be a better route to search for massive clusters in a wider redshift range. With the aim of discovering new radio halos and understanding their connection with cluster-cluster mergers, we have selected from the Planck Early source catalog the most massive clusters, and we have observed with the Giant Metrewave Radio Telescope at 323 MHz those objects for which deep observations were not available. We have discovered new peculiar radio emission in three of the observed clusters finding: (i) a radio halo in the cluster RXCJ0949.8+1708; (ii) extended emission in Abell 1443 that we classify as a radio halo plus a radio relic, with a bright filament embedded in the radio halo; (iii) low-power radio emission is found in CIZA J1938.3+5409 which is ten times below the radio - X-ray correlation, and represents the first direct detection of the radio emission in the "upper-limit" region of the radio - X-ray diagram. We discuss the properties of these new radio halos in the framework of theoretical models for the radio emission., 14 pages, 12 Figures, Accepted by MNRAS

We present adaptive optics-assisted integral field spectroscopy around the Hα or Hβ lines of 12 gravitationally lensed galaxies obtained with VLT/SINFONI,Keck/OSIRIS and Gemini/NIFS. We combine these data with previous observations and investigate the dynamics and star formation properties of 17 lensed galaxies at 1 < z

© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. We present adaptive optics-assisted integral field spectroscopy around the Hα or Hβ lines of 12 gravitationally lensed galaxies obtained with VLT/SINFONI,Keck/OSIRIS and Gemini/NIFS. We combine these data with previous observations and investigate the dynamics and star formation properties of 17 lensed galaxies at 1 < z⊙ yr-1, and stellar masses M* ~ 4 × 108-6 × 1010 M⊙. All of the galaxies show velocity gradients, with 59 per cent consistent with being rotating discs and a likely merger fraction of 29 per cent, with the remaining 12 per cent classed as 'undetermined'. We extract 50 star-forming clumps with sizes in the range 60 pc-1 kpc from the Hα (or Hβ) maps, and find that their surface brightnesses, Σclump and their characteristic luminosities, L0, evolve to higher luminosities with redshift. We show that this evolution can be described by fragmentation on larger scales in gas-rich discs, and is likely to be driven by evolving gas fractions.

International audience; We present adaptive optics-assisted integral field spectroscopy around the Halpha or Hbeta lines of 12 gravitationally lensed galaxies obtained with VLT/SINFONI, Keck/OSIRIS and Gemini/NIFS. We combine these data with previous observations and investigate the dynamics and star formation properties of 17 lensed galaxies at 1 < z < 4. Thanks to gravitational magnification of 1.4-90 times by foreground clusters, effective spatial resolutions of 40-700 pc are achieved. The magnification also allows us to probe lower star formation rates (SFRs) and stellar masses than unlensed samples; our target galaxies feature dust-corrected SFRs derived from Halpha or Hbeta emission of ˜0.8-40 M&sun; yr-1, and stellar masses M* ˜ 4 × 108-6 × 1010 M&sun;. All of the galaxies show velocity gradients, with 59 per cent consistent with being rotating discs and a likely merger fraction of 29 per cent, with the remaining 12 per cent classed as `undetermined'. We extract 50 star-forming clumps with sizes in the range 60 pc-1 kpc from the Halpha (or Hbeta) maps, and find that their surface brightnesses, Sigmaclump and their characteristic luminosities, L0, evolve to higher luminosities with redshift. We show that this evolution can be described by fragmentation on larger scales in gas-rich discs, and is likely to be driven by evolving gas fractions.

We present adaptive optics-assisted integral field spectroscopy around the Ha or Hb lines of 12 gravitationally lensed galaxies obtained with VLT/SINFONI, Keck/OSIRIS and Gemini/NIFS. We combine these data with previous observations and investigate the dynamics and star formation properties of 17 lensed galaxies at z = 1-4. Thanks to gravitational magnification of 1.4 - 90x by foreground clusters, effective spatial resolutions of 40 - 700 pc are achieved. The magnification also allows us to probe lower star formation rates and stellar masses than unlensed samples; our target galaxies feature dust-corrected SFRs derived from Ha or Hb emission of 0.8 - 40Msol/yr, and stellar masses M* ~ 4e8 - 6e10 Msol. All of the galaxies have velocity gradients, with 59% consistent with being rotating discs and a likely merger fraction of 29%, with the remaining 12% classed as 'undetermined.' We extract 50 star-forming clumps with sizes in the range 60pc - 1kpc from the Ha (or Hb) maps, and find that their surface brightnesses and their characteristic luminosities evolve to higher luminosities with redshift. We show that this evolution can be described by fragmentation on larger scales in gas-rich discs, and is likely to be driven by evolving gas fractions., 26 pages, 11 figures. Accepted for publication in MNRAS

We present adaptive optics-assisted integral field spectroscopy around the Hα or Hβ lines of 12 gravitationally lensed galaxies obtained with VLT/SINFONI,Keck/OSIRIS and Gemini/NIFS. We combine these data with previous observations and investigate the dynamics and star formation properties of 17 lensed galaxies at 1 < z

We report the discovery of a likely supernova (SN) at approximately 1 arcminute from the center of the galaxy cluster MACSJ0949.8+1708 (a.k.a. RXC J0949.8+1707, ZwCl 0947.2+1723).

We report the discovery of large-scale diffuse radio emission in the galaxy cluster MACS J1752.0+4440 (z = 0.366). Using Westerbork Synthesis Radio Telescope (WSRT) observa- tions we find that the cluster hosts a double radio relic system as well as a 1.65 Mpc radio halo covering the region between the two relics. The relics are diametrically located on opposite sides of the cluster centre. The NE and SW relics have sizes of 1.3 and 0.9 Mpc, respectively. In the case of an isolated binary merger event, the relative sizes of the relics suggest a mass ratio about 2:1. We measure integrated spectra of -1.16 ± 0.03 for the NE relic and -1.10 ± 0.05 for the SW relic. We conclude that this cluster has undergone a violent binary merger event and the relics are best explained by particles (re)accelerated in outwards travelling shock waves. The spectral indices suggest that the relics trace shock waves with Mach numbers (M) of around 3.5-4.5. These relatively high Mach numbers derived from the radio spectral index are comparable to those derived for a few other recently discovered relics. This implies that merger shocks with M > 3 are relatively common in cluster outskirts if our understanding of diffusive shock acceleration is correct. © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS.

We present Hubble Space Telescope/Wide Field Camera 3 narrow-band imaging of the Hα emission in a sample of eight gravitationally lensed galaxies at z = 1-1.5. The magnification caused by the foreground clusters enables us to obtain a median source plane spatial resolution of 360pc, as well as providing magnifications in flux ranging from ~10× to ~50×. This enables us to identify resolved star-forming Hii regions at this epoch and therefore study their Hα luminosity distributions for comparisons with equivalent samples at z ~ 2 and in the local Universe. We find evolution in the both luminosity and surface brightness of Hii regions with redshift. The distribution of clump properties can be quantified with an Hii region luminosity function, which can be fit by a power law with an exponential break at some cut-off, and we find that the cut-off evolves with redshift. We therefore conclude that 'clumpy' galaxies are seen at high redshift because of the evolution of the cut-off mass; the galaxies themselves follow similar scaling relations to those at z = 0, but their Hii regions are larger and brighter and thus appear as clumps which dominate the morphology of the galaxy. A simple theoretical argument based on gas collapsing on scales of the Jeans mass in a marginally unstable disc shows that the clumpy morphologies of high-z galaxies are driven by the competing effects of higher gas fractions causing perturbations on larger scales, partially compensated by higher epicyclic frequencies which stabilize the disc., RCL acknowledges a studentship from STFC, RGB and IS are supported by STFC and IS further acknowledges a Leverhulme Senior Fellowship. AMS acknowledges an STFC Advanced Fellowship, and JR is supported by the Marie Curie Career Integration Grant 294074. HE gratefully acknowledges financial support from STScI grants GO-09722, GO-10491, GO10875 and GO-12166. This work is based on observations with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for Program number 12197 and Program number 11678 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555

Recent measurements of large-scale peculiar velocities from the cumulative kinematic Sunyaev-Zel'dovich effect using WMAP data and X-ray selected clusters from ROSAT have identified a bulk flow of galaxy clusters at $\sim 600-1,000$ km s$^{-1}$ on scales of $\sim0.5-1$ Gpc, roughly aligned with the all-sky Cosmic Microwave Background (CMB) dipole. The flow is inferred from the detection of a residual dipole generated by CMB fluctuations exclusively in the direction of galaxy clusters, and measured within apertures containing zero monopole. Consistent with this interpretation, the amplitude of the dipole correlates with the X-ray luminosity of the clusters. To enable this measurement, the CMB data need to be filtered to remove the primary CMB, thereby increasing the data's signal-to-noise ratio. Filtering cannot imprint a signal with the mentioned properties at cluster positions; however, an inadequately designed filter can greatly suppress such a signal. We show here that recent studies that failed to detect a large-scale flow with various filters indeed adopted flawed implementations; when correctly implemented, these alternative filters lead to results that are in fact consistent with the Dark Flow signal. The discrepancies can be traced to the likely presence of residual dipoles caused by the thermal Sunyaev-Zel'dovich effect, to assumptions about cluster profiles incompatible with the data as well as failure to compute dipoles at the zero monopole aperture. PLANCK maps, with their large frequency coverage and a 217 GHz channel, will be instrumental to probe bulk flows, to remove spurious dipole signals and to help identify filtering schemes appropriate for this measurement., Revised arguments in section 3, results unchanged

We present HST/WFC3 narrowband imaging of the H-alpha emission in a sample of eight gravitationally-lensed galaxies at z = 1 - 1.5. The magnification caused by the foreground clusters enables us to obtain a median source plane spatial resolution of 360pc, as well as providing magnifications in flux ranging from ~10x to ~50x. This enables us to identify resolved star-forming HII regions at this epoch and therefore study their H-alpha luminosity distributions for comparisons with equivalent samples at z ~ 2 and in the local Universe. We find evolution in the both luminosity and surface brightness of HII regions with redshift. The distribution of clump properties can be quantified with an HII region luminosity function, which can be fit by a power law with an exponential break at some cut-off, and we find that the cut-off evolves with redshift. We therefore conclude that `clumpy' galaxies are seen at high redshift because of the evolution of the cut-off mass; the galaxies themselves follow similar scaling relations to those at z = 0, but their HII regions are larger and brighter and thus appear as clumps which dominate the morphology of the galaxy. A simple theoretical argument based on gas collapsing on scales of the Jeans mass in a marginally unstable disk shows that the clumpy morphologies of high-z galaxies are driven by the competing effects of higher gas fractions causing perturbations on larger scales, partially compensated by higher epicyclic frequencies which stabilise the disk., Comment: 16 pages, 9 figures, 2 tables, accepted for publication in MNRAS

We report the discovery of large-scale diffuse radio emission in the galaxy cluster MACS J1752.0+4440 (z=0.366). Using Westerbork Synthesis Radio Telescope (WSRT) observations we find that the cluster hosts a double radio relic system as well as a 1.65 Mpc radio halo covering the region between the two relics. The relics are diametrically located on opposite sides of the cluster center. The NE and SW relics have sizes of 1.3 and 0.9 Mpc, respectively. In case of an isolated binary merger event, the relative sizes of the relics suggest a mass ratio about 2:1. We measure integrated spectra of -1.16 \pm 0.03 for the NE and -1.10 \pm 0.05 for the SW relic. We conclude that this cluster has undergone a violent binary merger event and the relics are best explained by particles (re)accelerated in outwards traveling shock waves. The spectral indices suggest the relics trace shock waves with Mach numbers (M) of around 3.5 to 4.5. These relatively high Mach numbers derived from the radio spectral index are comparable to those derived for a few other recently discovered relics. This implies that merger shocks with M > 3 are relatively common in cluster outskirts if our understanding of diffusive shock acceleration is correct., 6 pages, 3 figures, accepted for publication in MNRAS

We present the first statistical study of X-ray cavities in distant clusters of galaxies (z > 0.3). With the aim of providing further insight into how active galactic nucleus (AGN) feedback operates at higher redshift, we have analysed the Chandra X-ray observations of the MAssive Cluster Survey (MACS) and searched for surface brightness depressions associated with the brightest cluster galaxy (BCG). The MACS sample consists of the most X-ray luminous clusters within 0.3 ≤z≤ 0.7 (median LX, RASS= 7 × 1044 erg s−1), and out of 76 clusters, we find 13 with ‘clear’ cavities and seven with ‘potential’ cavities (detection rate ∼25 per cent). Most of the clusters in which we find cavities have a short central cooling time below 3–5 Gyr, consistent with the idea that cavities sit predominantly in cool core clusters. We also find no evidence for evolution in any of the cavity properties with redshift, up to z∼ 0.6. The cavities of powerful outbursts are not larger (or smaller) at higher redshift, and are not able to rise to further (or lesser) distances from the nucleus. The energetics of these outbursts also remain the same. This suggests that extreme ‘radio mode’ feedback (Lmech > 1044 erg s−1) starts to operate as early as 7–8 Gyr after the big bang and shows no sign of evolution since then. In other words, AGNs lying at the centre of clusters are able to operate at early times with extreme mechanical powers, and have been operating in such a way for at least the past 5 Gyr.

In this review we present a comprehensive discussion of peculiar velocity field measured recently on very large scales with a novel method using X-ray galaxy clusters as tracers. The measurement is based on the kinematic component of the Sunyaev-Zeldovich (KSZ) effect produced by Compton scattering of cosmic microwave background (CMB) photons off the hot intracluster gas, and uses a large catalog of X-ray selected clusters and all-sky CMB maps obtained with the WMAP satellite. The method probes the dipole of the CMB temperature field evaluated at the cluster positions and within the apertures in which the CMB monopole contribution vanishes, thereby isolating the signal remaining from the KSZ effect produced by coherently moving clusters. The detection of a highly significant dipole out to the depth of at least ~ 800 Mpc casts doubt on the notion that gravitational instability from the observed mass distribution is the sole -- or even dominant -- cause of the detected motions. Rather it appears that the flow may extend across the entire observable Universe. Possible implications include the possibility to constrain the primeval preinflationary structure of space-time and its landscape, and/or the need for modifications of presently known physics (e.g. arising from a higher-dimensional structure of gravity). We review these possibilities in light of the measurements described here and specifically discuss the prospects of future measurements and the issues they should resolve. We address the consistency of these large-scale velocity measurements with those obtained on smaller scales by studies using galaxies as tracers, and resolve the discrepancies with two recent claims based on modified CMB analysis schemes., Physics Reports, draft version - comments welcome! Manuscript with all figures at full resolution is available from http://www.kashlinsky.info/bulkflows/physicsreport

We present the results of a simple but robust morphological classification of a statistically complete sample of 108 of the most X-ray-luminous clusters at 0.15 ≤z≤ 0.7 observed with Chandra. Our aims are to (a) identify the most disturbed massive clusters to be used as gravitational lenses for studies of the distant Universe and as probes of particle acceleration mechanisms resulting in non-thermal radio emission; (b) find cluster mergers featuring subcluster trajectories that make them suitable for quantitative analyses of cluster collisions; and (c) constrain the evolution with redshift of the cluster merger fraction. Finally, (d) this paper represents the third public release of clusters from the MAssive Cluster Survey sample, adding 24 clusters to the 46 published previously. To classify clusters by the degree of relaxation, we use the projected offset of the brightest cluster galaxy from the peak (or the global centroid) of the X-ray emission as a measure of the segregation between the intracluster gas and dark matter, and also perform a visual assessment of the optical and X-ray morphology on all scales. Regarding (a), we identify 10 complex systems likely to have undergone multiple merger events in the recent past. Regarding (b), we identify 11 systems likely to be post-collision, binary, head-on mergers (BHOMs), as well as another six mergers that are possible BHOMs but probably harder to interpret because of non-negligible impact parameters and merger axes closer to our line of sight. Regarding (c), we find a highly significant increase with redshift in the fraction of morphologically disturbed clusters (and thus a clear decrease in the number of fully relaxed systems) starting at z∼ 0.4, in spite of a detection bias in our sample against very disturbed systems at high redshift. Since our morphological diagnostics are all based on imaging data and thus sensitive to projection effects, the measured merger fractions should be considered lower limits and our list of mergers incomplete, as we are likely to miss systems forming along axes close to our line of sight. A larger sample of clusters with high-quality X-ray data in particular at high redshift will be needed to trace the evolutionary history of cluster growth and relaxation closer to the primary epoch of cluster formation z∼ 1.

We present the first statistical study of X-ray cavities in distant clusters of galaxies (z > 0.3). With the aim of providing further insight into how AGN feedback operates at higher redshift, we have analysed the Chandra X-ray observations of the Massive Cluster Survey (MACS) and searched for surface-brightness depressions associated with the Brightest Cluster Galaxy (BCG). The MACS sample consists of the most X-ray luminous clusters within 0.3 < z < 0.7 (median L_(X,RASS) = 7*10^44 erg/s), and out of 76 clusters, we find 13 with "clear" cavities and 7 with "potential" cavities (detection rate ~25 per cent). Most of the clusters in which we find cavities have a short central cooling time below 3 - 5 Gyrs, consistent with the idea that cavities sit predominantly in cool core clusters. We also find no evidence for evolution in any of the cavity properties with redshift, up to z~0.6. The cavities of powerful outbursts are not larger (or smaller) at higher redshift, and are not able to rise to further (or lesser) distances from the nucleus. The energetics of these outbursts also remain the same. This suggests that extreme "radio mode" feedback (L_(mech) > 10^44 erg/s) starts to operate as early as 7 - 8 Gyrs after the Big Bang and shows no sign of evolution since then. In other words, AGNs lying at the centre of clusters are able to operate at early times with extreme mechanical powers, and have been operating in such a way for at least the past 5 Gyrs., Comment: 27 pages, 14 figures, 4 tables, accepted for publication in MNRAS. A pdf version of the paper with high-resolution images can be found at http://www-xray.ast.cam.ac.uk/~juliehl/MACSpaper/

We present a statistically complete sample of very X-ray luminous galaxy clusters detected in the MAssive Cluster Survey (MACS). This second MACS release comprises all 34 MACS clusters with nominal X-ray fluxes in excess of 2x10^(-12) erg/s/cm^2 (0.1-2.4 keV) in the ROSAT Bright Source Catalogue; two thirds of them are new discoveries. Extending over the redshift range from 0.3 to 0.5, this subset complements the complete sample of the 12 most distant MACS clusters (z>0.5) published in 2007 and further exemplifies the efficacy of X-ray selection for the compilation of samples of intrinsically massive galaxy clusters. Extensive follow-up observations with Chandra/ACIS led to three additional MACS cluster candidates being eliminated as (predominantly) X-ray point sources. For another four clusters --- which, however, remain in our sample of 34 --- the point-source contamination was found to be about 50%. The median X-ray luminosity of 1.3x10^45 erg/s (0.1-2.4 keV, Chandra, within r_500) of the clusters in this subsample demonstrates the power of the MACS survey strategy to find the most extreme and rarest clusters out to significant redshift. A comparison of the optical and X-ray data for all clusters in this release finds a wide range of morphologies with no obvious bias in favour of either relaxed or merging systems., 10 pages, 6 figures, 2 tables; accepted for publication in MNRAS

We use an 18' x 9' mosaic of ACS images covering the entire large-scale structure around the X-ray luminous cluster MACSJ0717.5 (z=0.545) to study the morphology of galaxies at the cluster redshift. We find the global fraction of morphological types of galaxies to be consistent with results in the literature. Interestingly, we find that the fraction of S0s also correlates with local galaxy density, in contrast to the findings of a study of the cores of 10 clusters at similar redshift by Dressler et al. We suggest that this apparent inconsistency is due to differences in the spatial coverage around clusters, which is supported by the fact that the correlation disappears for S0s within a radius of 0.6R_200 of MACSJ0717. We interpret this result as evidence of the morphology-density relation being caused by a combination of morphological transformation triggered by galaxy-galaxy interactions, and effects related to the formation and evolution of large-scale structure. In environments of low to intermediate density, where galaxy-galaxy interactions are frequent and efficient, the observed pronounced morphology-density relation for S0s reflects the density dependence of the interaction cross section. In clusters, however, the correlation disappears for S0s, as the much higher galaxy velocities in clusters not only lower the interaction cross section, but also cause a spatial redistribution of galaxies that all but destroys such a correlation. This argument does not hold for elliptical galaxies in clusters which, having formed much earlier, have settled into the large-scale cluster potential; hence the morphology-density relation for cluster ellipticals may reflect primarily the state of advanced dynamical relaxation of this population within the cluster rather than a causal link to the environment responsible for the morphological transformation of galaxies., Comment: accepted by MNRAS; Full resolution version of fig 1 and fig 2 will be published in the journal

We present results of an extensive morphological, spectroscopic, and photometric study of the galaxy population of MACS J0025.4$-$1225 (z=0.586), a major cluster merger with clear segregation of dark and luminous matter, to examine the impact of mergers on galaxy evolution. Based on 436 galaxy spectra obtained with Keck DEIMOS, we identified 212 cluster members within 4 Mpc of the cluster centre, and classified them using three spectroscopic types; we find 111 absorption-line, 90 emission-line (including 23 e(a) and 11 e(b)), and 6 E+A galaxies. The fraction of absorption(emission)-line galaxies is a monotonically increasing(decreasing) function of both projected galaxy density and radial distance to the cluster center. More importantly, the 6 observed E+A cluster members are all located between the dark-matter peaks of the cluster and within ~0.3Mpc radius of the X-ray flux peak, unlike the E+A galaxies in other intermediate-redshift clusters which are usually found to avoid the core region. In addition, we use Hubble Space Telescope imaging to classify cluster members according to morphological type. We find the global fraction of spiral and lenticular galaxies in MACS J0025 to be among the highest observed to date in clusters at z>0.5. The observed E+A galaxies are found to be of lenticular type with Sersic indices of ~2, boosting the local fraction of S0 to 70 per cent between the dark-matter peaks. Combing the results of our analysis of the spatial distribution, morphology, and spectroscopic features of the galaxy population, we propose that the starburst phase of these E+A galaxies was both initiated and terminated during the first core-passage about 0.5--1Gyr ago, and that their morphology has already been transformed into S0 due to ram pressure and/or tidal forces near the cluster core. By contrast, ongoing starbursts are observed predominantly in infalling galaxies, and thus appears to be unrelated to the cluster merger., 18 pages, 17 figures, accepted by MNRAS

Although autism is a highly heritable neurodevelopmental disorder, attempts to identify specific susceptibility genes have thus far met with limited success. Genome-wide association studies using half a million or more markers, particularly those with very large sample sizes achieved through meta-analysis, have shown great success in mapping genes for other complex genetic traits. Consequently, we initiated a linkage and association mapping study using half a million genome-wide single nucleotide polymorphisms (SNPs) in a common set of 1,031 multiplex autism families (1,553 affected offspring). We identified regions of suggestive and significant linkage on chromosomes 6q27 and 20p13, respectively. Initial analysis did not yield genome-wide significant associations; however, genotyping of top hits in additional families revealed an SNP on chromosome 5p15 (between SEMA5A and TAS2R1) that was significantly associated with autism (P = 2 × 10-7). We also demonstrated that expression of SEMA5A is reduced in brains from autistic patients, further implicating SEMA5A as an autism susceptibility gene. The linkage regions reported here provide targets for rare variation screening whereas the discovery of a single novel association demonstrates the action of common variants.

Using WMAP 3-year data at the locations of close to $\sim 700$ X-ray selected clusters we have detected the amplitude of the thermal Sunyaev-Zeldovich (TSZ) effect at the 15$\sigma$ level, the highest statistical significance reported so far. Owing to the large size of our cluster sample, we are able to detect the corresponding CMB distortions out to large cluster-centric radii. The region over which the TSZ signal is detected is, on average, four times larger in radius than the X-ray emitting region, extending to $\sim 3h_{70}^{-1}$Mpc. We show that an isothermal $\beta$ model does not fit the electron pressure at large radii; instead, the baryon profile is consistent with the Navarro-Frenk-White profile, expected for dark matter in the concordance $\Lambda$CDM model. The X-ray temperature at the virial radius of the clusters falls by a factor $\sim 3-4$ from the central value, depending on the cluster concentration parameter. Our results suggest that cluster dynamics at large radii is dominated by dark matter and is well described by Newtonian gravity., Comment: ApJ Lett, to be published on March 10th, 2008

We present constraints on the mean matter density, Omega_m, dark energy density, Omega_de, and the dark energy equation of state parameter, w, using Chandra measurements of the X-ray gas mass fraction (fgas) in 42 hot (kT>5keV), X-ray luminous, dynamically relaxed galaxy clusters spanning the redshift range 0.05, Comment: Published in MNRAS. 20 pages, 11 figures. The data and analysis code (in the form of a patch to CosmoMC) are now available at http://www.stanford.edu/~drapetti/fgas_module/

We present the statistically complete and cosmologically most relevant subset of the twelve most distant galaxy clusters detected at z>0.5 by the MAssive Cluster Survey (MACS). Ten of these systems are new discoveries; only two (MACSJ0018.5+1626 aka CL0016+1609, and MACSJ0454.1-0300 aka MS0451.6-0305) were previously known. We provide fundamental cluster properties derived from our optical and X-ray follow-up observations as well as the selection function in tabulated form to facilitate cosmological studies using this sample., Comment: Four pages, 1 figure, submitted to ApJ

40 pages, 17 figures, high resolution draft at http://www.dark-cosmology.dk/~marceau/1689.pdf; astro-ph/0612165; We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z = 0.18 using detected strong lensing features from deep HST/ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 24 multiply imaged systems with newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems. The resultant mass model enables us to reliably predict the redshifts of additional multiply imaged systems for which no spectra are currently available, and to use the location of these systems to further constrain the mass model. In particular, we have detected 5 strong galaxy-galaxy lensing systems just outside the Einstein ring region, further constraining the mass profile. Our strong lensing mass model is consistent with that inferred from our large scale weak lensing analysis derived using CFH12k wide field images. Thanks to a new method for reliably selecting a well defined background lensed galaxy population, we resolve the discrepancy found between the strong and weak lensing mass models reported in earlier work. [ABRIDGED]

We present the statistically complete and cosmologically most relevant subset of the twelve most distant galaxy clusters detected at z>0.5 by the MAssive Cluster Survey (MACS). Ten of these systems are new discoveries; only two (MACSJ0018.5+1626 aka CL0016+1609, and MACSJ0454.1-0300 aka MS0451.6-0305) were previously known. We provide fundamental cluster properties derived from our optical and X-ray follow-up observations as well as the selection function in tabulated form to facilitate cosmological studies using this sample., Four pages, 1 figure, submitted to ApJ

Aims: We present a wide-field multi-color survey of a homogeneous sample of eleven clusters of galaxies for which we measure total masses and mass distributions from weak lensing. Methods: The eleven clusters in our sample are all X-ray luminous and span a narrow redshift range at z=0.21 +/- 0.04. The weak lensing analysis of the sample is based on ground-based wide-field imaging obtained with the CFH12k camera on CFHT. We use the methodology developed and applied previously on the massive cluster Abell 1689. A Bayesian method, implemented in the Im2shape software, is used to fit the shape parameters of the faint background galaxies and to correct for PSF smearing. With the present data, shear profiles are measured in all clusters out to at least 2 Mpc (more than 15arcmin from the center) with high confidence. The radial shear profiles are fitted with different parametric mass profiles and the virial mass M_200 is estimated for each cluster and then compared to other physical properties. Results: Scaling relations between mass and optical luminosity indicate an increase of the M/L ratio with luminosity and a L_X-M_200 relation scaling as L_X \propto M_200^(0.83 +/- 0.11) while the normalization of the M_200 \propto T_X^{3/2} relation is close to the one expected from hydrodynamical simulations of cluster formation as well as previous X-ray analyses. We suggest that the dispersion in the M_200-T_X and M_200-L_X relations reflects the different merging and dynamical histories for clusters of similar X-ray luminosities and intrinsic variations in their measured masses. Improved statistics of clusters over a wider mass range are required for a better control of the intrinsic scatter in scaling relations., Comment: 20 pages, 11 figures, revised version now accepted to Astronomy and Astrophysics. Full version with high resolution figures at http://www.ast.obs-mip.fr/users/soucail/highlx.pdf

The X-ray properties of a sample of 11 high-redshift (0.61 or in the early stages of the clusters' formation, prior to their observation. The properties of the intra-cluster medium at high-redshift are found to be similar to those in the local universe. The mean surface-brightness profile slope for the sample is 0.66+/-0.05, the mean gas mass fractions within R2500 and R200 are 0.073+/-0.010 and 0.12+/-0.02 respectively, and the mean metallicity of the sample is 0.28+/-0.16 solar., Comment: 23 pages, 17 figures. Accepted for publication in MNRAS. Revised to match accepted version: reanalysed data with latest calibrations, several minor changes. Conclusions unchanged

The X-ray properties of a sample of 11 high-redshift (0.61 or in the early stages of the clusters' formation, prior to their observation. The properties of the intra-cluster medium at high-redshift are found to be similar to those in the local universe. The mean surface-brightness profile slope for the sample is 0.66+/-0.05, the mean gas mass fractions within R2500 and R200 are 0.073+/-0.010 and 0.12+/-0.02 respectively, and the mean metallicity of the sample is 0.28+/-0.16 solar., 23 pages, 17 figures. Accepted for publication in MNRAS. Revised to match accepted version: reanalysed data with latest calibrations, several minor changes. Conclusions unchanged