The Kepler-454 system: a small, not-rocky inner planet, a Jovian world, and a distant companion

Kepler-454 (KOI-273) is a relatively bright (V = 11.69 mag), Sun-like star that hosts a transiting planet candidate in a 10.6 day orbit. From spectroscopy, we estimate the stellar temperature to be 5687 ± 50 K, its metallicity to be [m/H] = 0.32 ± 0.08, and the projected rotational velocity to be v sin i <2.4 km s^-1. We combine these values with a study of the asteroseismic frequencies from short cadence Kepler data to estimate the stellar mass to be , the radius to be 1.066 ± 0.012 R_o, and the age to be Gyr. We estimate the radius of the 10.6 day planet as 2.37 ± 0.13 R_⊕. Using 63 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 36 observations made with the HIRES spectrograph at the Keck Observatory, we measure the mass of this planet to be 6.8 ± 1.4 M_⊕. We also detect two additional non-transiting companions, a planet with a minimum mass of 4.46 ± 0.12 M_J in a nearly circular 524 day orbit and a massive companion with a period >10 years and mass >12.1 M_J. The 12 exoplanets with radii ⊕ and precise mass measurements appear to fall into two populations, with those ⊕ following an Earth-like composition curve and larger planets requiring a significant fraction of volatiles. With a density of 2.76 ± 0.73 g cm^-3, Kepler-454b lies near the mass transition between these two populations and requires the presence of volatiles and/or H/He gas.

The HARPS-N Rocky Planet Search. I. HD 219134 b: A transiting rocky planet in a multi-planet system at 6.5 pc from the Sun

We know now from radial velocity surveys and transit space missions thatplanets only a few times more massive than our Earth are frequent aroundsolar-type stars. Fundamental questions about their formation history,physical properties, internal structure, and atmosphere composition are,however, still to be solved. We present here the detection of a systemof four low-mass planets around the bright (V = 5.5) and close-by (6.5pc) star HD 219134. This is the first result of the Rocky Planet Searchprogramme with HARPS-N on the Telescopio Nazionale Galileo in La Palma.The inner planet orbits the star in 3.0935 ± 0.0003 days, on aquasi-circular orbit with a semi-major axis of 0.0382 ± 0.0003AU. Spitzer observations allowed us to detect the transit of the planetin front of the star making HD 219134 b the nearest known transitingplanet to date. From the amplitude of the radial velocity variation(2.25 ± 0.22 ms-1) and observed depth of the transit(359 ± 38 ppm), the planet mass and radius are estimated to be4.36 ± 0.44 M⊕ and 1.606 ± 0.086R⊕, leading to a mean density of 5.76 ± 1.09 gcm-3, suggesting a rocky composition. One additional planetwith minimum-mass of 2.78 ± 0.65 M⊕ moves on aclose-in, quasi-circular orbit with a period of 6.767 ± 0.004days. The third planet in the system has a period of 46.66 ± 0.08days and a minimum-mass of 8.94 ± 1.13 M⊕, at0.233 ± 0.002 AU from the star. Its eccentricity is 0.46 ±0.11. The period of this planet is close to the rotational period of thestar estimated from variations of activity indicators (42.3 ± 0.1days). The planetary origin of the signal is, however, thepreferredsolution as no indication of variation at the corresponding frequency isobserved for activity-sensitive parameters. Finally, a fourth additionallonger-period planet of mass of 71 M⊕ orbits the starin 1842 days, on an eccentric orbit (e = 0.34 ± 0.17) at adistance of 2.56 AU.The photometric time series and radial velocities used in this work areavailable in electronic form at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/584/A72

The Mass of Kepler-93b and The Composition of Terrestrial Planets

Kepler-93b is a 1.478 ± 0.019 R ⊕ planet with a4.7 day period around a bright (V = 10.2), astroseismicallycharacterized host star with a mass of 0.911 ± 0.033 M⊙ and a radius of 0.919 ± 0.011 R⊙. Based on 86 radial velocity observations obtainedwith the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 32archival Keck/HIRES observations, we present a precise mass estimate of4.02 ± 0.68 M ⊕. The corresponding high densityof 6.88 ± 1.18 g cm-3 is consistent with a rockycomposition of primarily iron and magnesium silicate. We compareKepler-93b to other dense planets with well-constrained parameters andfind that between 1 and 6 M ⊕, all dense planetsincluding the Earth and Venus are well-described by the same fixed ratioof iron to magnesium silicate. There are as of yet no examples of suchplanets with masses >6 M ⊕. All known planets inthis mass regime have lower densities requiring significant fractions ofvolatiles or H/He gas. We also constrain the mass and period of theouter companion in the Kepler-93 system from the long-term radialvelocity trend and archival adaptive optics images. As the sample ofdense planets with well-constrained masses and radii continues to grow,we will be able to test whether the fixed compositional model found forthe seven dense planets considered in this paper extends to the fullpopulation of 1-6 M ⊕ planets.Based on observations made with the Italian Telescopio Nazionale Galileo(TNG) operated on the island of La Palma by the Fundación GalileoGalilei of the INAF (Istituto Nazionale di Astrofisica) at the SpanishObservatorio del Roque de los Muchachos of the Instituto de Astrofisicade Canarias.

The VLT-FLAMES Tarantula survey: XX. The nature of the X-ray bright emission-line star VFTS 399

Context: The stellar population of the 30 Doradus star-forming region in the Large Magellanic Cloud contains a subset of apparently single, rapidly rotating O-type stars. The physical processes leading to the formation of this cohort are currently uncertain. 

Aims: One member of this group, the late O-type star VFTS 399, is found to be unexpectedly X-ray bright for its bolometric luminosity-in this study we aim to determine its physical nature and the cause of this behaviour. 

Methods: To accomplish this we performed a time-resolved analysis of optical, infrared and X-ray observations. 

Results: We found VFTS 399 to be an aperiodic photometric variable with an apparent near-IR excess. Its optical spectrum demonstrates complex emission profiles in the lower Balmer series and select He i lines-taken together these suggest an OeBe classification. The highly variable X-ray luminosity is too great to be produced by a single star, while the hard, non-thermal nature suggests the presence of an accreting relativistic companion. Finally, the detection of periodic modulation of the X-ray lightcurve is most naturally explained under the assumption that the accretor is a neutron star. 

Conclusions: VFTS 399 appears to be the first high-mass X-ray binary identified within 30 Dor, sharing many observational characteristics with classical Be X-ray binaries. Comparison of the current properties of VFTS 399 to binary-evolution models suggests a progenitor mass 25 M_⊙ for the putative neutron star, which may host a magnetic field comparable in strength to those of magnetars. VFTS 399 is now the second member of the cohort of rapidly rotating "single" O-type stars in 30 Dor to show evidence of binary interaction resulting in spin-up, suggesting that this may be a viable evolutionary pathway for the formation of a subset of this stellar population.

Detection of H2O and Evidence for TiO/VO in an Ultra-hot Exoplanet Atmosphere

We present a primary transit observation for the ultra-hot (T eq ~ 2400 K) gas giant expolanet WASP-121b, made using the Hubble Space Telescope Wide Field Camera 3 in spectroscopic mode across the 1.12–1.64 μm wavelength range. The 1.4 μm water absorption band is detected at high confidence (5.4σ) in the planetary atmosphere. We also reanalyze ground-based photometric light curves taken in the B, r', and z' filters. Significantly deeper transits are measured in these optical bandpasses relative to the near-infrared wavelengths. We conclude that scattering by high-altitude haze alone is unlikely to account for this difference and instead interpret it as evidence for titanium oxide and vanadium oxide absorption. Enhanced opacity is also inferred across the 1.12–1.3 μm wavelength range, possibly due to iron hydride absorption. If confirmed, WASP-121b will be the first exoplanet with titanium oxide, vanadium oxide, and iron hydride detected in transmission. The latter are important species in M/L dwarfs and their presence is likely to have a significant effect on the overall physics and chemistry of the atmosphere, including the production of a strong thermal inversion.

An extreme planetary system around HD 219828: one long-period super Jupiter to a hot-Neptune host star

Context. With about 2000 extrasolar planets confirmed, the results show that planetary systems have a whole range of unexpected properties. This wide diversity provides fundamental clues to the processes of planet formation and evolution. Aims: We present a full investigation of the HD 219828 system, a bright metal-rich star for which a hot Neptune has previously been detected. Methods: We used a set of HARPS, SOPHIE, and ELODIE radial velocities to search for the existence of orbiting companions to HD 219828. The spectra were used to characterise the star and its chemical abundances, as well as to check for spurious, activity induced signals. A dynamical analysis is also performed to study the stability of the system and to constrain the orbital parameters and planet masses. Results: We announce the discovery of a long period (P = 13.1 yr) massive (m sini = 15.1 MJup) companion (HD 219828 c) in a very eccentric orbit (e = 0.81). The same data confirms the existence of a hot Neptune, HD 219828 b, with a minimum mass of 21 M⊕ and a period of 3.83 days. The dynamical analysis shows that the system is stable, and that the equilibrium eccentricity of planet b is close to zero. Conclusions: The HD 219828 system is extreme and unique in several aspects. First, ammong all known exoplanet systems it presents an unusually high mass ratio. We also show that systems like HD 219828, with a hot Neptune and a long-period massive companion are more frequent than similar systems with a hot Jupiter instead. This suggests that the formation of hot Neptunes follows a different path than the formation of their hot jovian counterparts. The high mass, long period, and eccentricity of HD 219828 c also make it a good target for Gaia astrometry as well as a potential target for atmospheric characterisation, using direct imaging or high-resolution spectroscopy. Astrometric observations will allow us to derive its real mass and orbital configuration. If a transit of HD 219828 b is detected, we will be able to fully characterise the system, including the relative orbital inclinations. With a clearly known mass, HD 219828 c may become a benchmark object for the range in between giant planets and brown dwarfs.

Is the activity level of HD 80606 influenced by its eccentric planet?

Aims: Several studies suggest that the activity level of a planet-host star can be influenced by the presence of a close-by orbiting planet. Moreover, the interaction mechanisms that have been proposed, magnetic interaction and tidal interaction, exhibit a very different dependence on the orbital separation between the star and the planet. A detection of activity enhancement and characterization of its dependence on planetary orbital distance can, in principle, allow us to characterize the physical mechanism behind the activity enhancement. Methods: We used the HARPS-N spectrograph to measure the stellar activity level of HD 80606 during the planetary periastron passage and compared the activity measured to that close to apastron. Being characterized by an eccentricity of 0.93 and an orbital period of 111 days, the system's extreme variation in orbital separation makes it a perfect target to test our hypothesis. Results: We find no evidence for a variation in the activity level of the star as a function of planetary orbital distance, as measured by all activity indicators employed: log(R'HK), Hα, NaI, and HeI. None of the models employed, whether magnetic interaction or tidal interaction, provides a good description of the data. The photometry revealed no variation either, but it was strongly affected by poor weather conditions. Conclusions: We find no evidence for star-planet interaction in HD 80606 at the moment of the periastron passage of its very eccentric planet. The straightforward explanation for the non-detection is the absence of interaction as a result of a low magnetic field strength on either the planet or the star and of the low level of tidal interaction between the two. However, we cannot exclude two scenarios: i) the interaction can be instantaneous and of magnetic origin, being concentrated on the substellar point and its surrounding area; and ii) the interaction can lead to a delayed activity enhancement. In either scenario, a star-planet interaction would not be detectable with the dataset described in this paper.

Effort-reward imbalance and sedentary lifestyle: an observational study in a large occupational cohort

Objectives: To investigate the association between effort-reward imbalance (ERI) at work and sedentary lifestyle. Methods: Cross-sectional data from the ongoing Finnish Public Sector Study related to 30 433 women and 7718 men aged 17-64 were used (n = 35 918 after exclusion of participants with missing values in covariates). From the responses to a questionnaire, an aggregated mean score for ERI in a work unit was assigned to each participant. The outcome was sedentary lifestyle defined as <2.00 metabolic equivalent task (MET) hours/day. Logistic regression with generalized estimating equations was used as an analysis method to include both individual and work unit level predictors in the models. Adjustments were made for age, marital status, occupational status, job contract, smoking, and heavy drinking. Results: Twenty five percent of women and 27% of men had a sedentary lifestyle. High individual level ERI was associated with a higher likelihood of sedentary lifestyle both among women (odds ratio (OR) = 1.08, 95% CI 1.01 to 1.16) and men (OR = 1.17, 95% CI 1.02 to 1.33). These associations were not explained by relevant confounders and they were also independent of work unit level job strain measured as a ratio of job demands and control. Conclusions: A mismatch between high occupational effort spent and low reward received in turn seems to be associated with an elevated risk of sedentary lifestyle, although this association is relatively weak.

Effort-reward imbalance at work and the co-occurrence of lifestyle risk factors: cross-sectional survey in a sample of 36,127 public sector employees

Background In occupational life, a mismatch between high expenditure of effort and receiving few rewards may promote the co-occurrence of lifestyle risk factors, however, there is insufficient evidence to support or refute this hypothesis. The aim of this study is to examine the extent to which the dimensions of the Effort-Reward Imbalance (ERI) model – effort, rewards and ERI – are associated with the co-occurrence of lifestyle risk factors. Methods Based on data from the Finnish Public Sector Study, cross-sectional analyses were performed for 28,894 women and 7233 men. ERI was conceptualized as a ratio of effort and rewards. To control for individual differences in response styles, such as a personal disposition to answer negatively to questionnaires, occupational and organizational -level ecological ERI scores were constructed in addition to individual-level ERI scores. Risk factors included current smoking, heavy drinking, body mass index ≥25 kg/m2, and physical inactivity. Multinomial logistic regression models were used to estimate the likelihood of having one risk factor, two risk factors, and three or four risk factors. The associations between ERI and single risk factors were explored using binary logistic regression models. Results After adjustment for age, socioeconomic position, marital status, and type of job contract, women and men with high ecological ERI were 40% more likely to have simultaneously ≥3 lifestyle risk factors (vs. 0 risk factors) compared with their counterparts with low ERI. When examined separately, both low ecological effort and low ecological rewards were also associated with an elevated prevalence of risk factor co-occurrence. The results obtained with the individual-level scores were in the same direction. The associations of ecological ERI with single risk factors were generally less marked than the associations with the co-occurrence of risk factors. Conclusion This study suggests that a high ratio of occupational efforts relative to rewards may be associated with an elevated risk of having multiple lifestyle risk factors. However, an unexpected association between low effort and a higher likelihood of risk factor co-occurrence as well as the absence of data on overcommitment (and thereby a lack of full test of the ERI model) warrant caution in regard to the extent to which the entire ERI model is supported by our evidence.

The metal content of bulge field stars from FLAMES-GIRAFFE spectra - I. Stellar parameters and iron abundances

Aims. We determine the iron distribution function (IDF) for bulge field stars, in three different fields along the Galactic minor axis and at latitudes b = -4 degrees, b = -6 degrees, and b = -12 degrees. A fourth field including NGC 6553 is also included in the discussion. Methods. About 800 bulge field K giants were observed with the GIRAFFE spectrograph of FLAMES@VLT at spectral resolution R similar to 20 000. Several of them were observed again with UVES at R similar to 45 000 to insure the accuracy of the measurements. The LTE abundance analysis yielded stellar parameters and iron abundances that allowed us to construct an IDF for the bulge that, for the first time, is based on high-resolution spectroscopy for each individual star. Results. The IDF derived here is centered on solar metallicity, and extends from [Fe/H] similar to -1.5 to [Fe/H] similar to + 0.5. The distribution is asymmetric, with a sharper cutoff on the high-metallicity side, and it is narrower than previously measured. A variation in the mean metallicity along the bulge minor axis is clearly between b = -4 degrees and b = -6 degrees ([Fe/H] decreasing similar to by 0.6 dex per kpc). The field at b = -12 degrees. is consistent with the presence of a gradient, but its quantification is complicated by the higher disk/bulge fraction in this field. Conclusions. Our findings support a scenario in which both infall and outflow were important during the bulge formation, and then suggest the presence of a radial gradient, which poses some challenges to the scenario in which the bulge would result solely from the vertical heating of the bar.

A type stars - physical parameters from UVBY and H-beta photometry

uvby H-beta photometry has been obtained for a sample of 93 selected main sequence A stars. The purpose was to determine accurate effective temperatures, surface gravities, and absolute magnitudes for an individual determination of ages and parallaxes, which have to be included in a more extensive work analyzing the kinematic properties of A V stars. Several calibrations and methods to determine the above mentioned parameters have been reviewed, allowing the design of a new algorithm for their determination. The results obtained using this procedure were tested in a previous paper using uvby H-beta data from the Hauck and Mermilliod catalogue, and comparing the rusulting temperatures, surface gravities and absolute magnitudes with empirical determinations of these parameters.

Individual Perception of Organizational Values

The objective of this master’s thesis was to examine how corporate values come true among the white-collar employees in the case organization. It was also studied if values were perceived similarly in the different departments. Impact of organizational position and education on value orientation was tested through hypotheses based on earlier values research. There are only few value scales available for measuring organizational values. The empirical study results indicate that personnel’s perception of organizational values can be measured statistically. When defining the scale it is utmost important to link the questions and claims close to the employees’ daily working environment. In this study, Work ethic appeared as the strongest organizational value reflecting respondents’ commitment to their duties. Related to corporate values, Performance was perceived as the strongest value and Emphasis on people the weakest. Value consensus between the departments varied. According to the previous research organizational position and educational level has an impact on value perceptions. In this study, employees in superior position or with higher education perceived organizational values to come true better than subordinates or employees with lower education. Empirical data (N=229) was collected by a web-based survey questionnaire among white-collar employees in the case organization in April 2008. Statistical analyses were performed by SPSS programme.

Yhtiöittämisen näkyminen työtyytyväisyydessä muutosprosessin eri vaiheissa

Tutkimuksessa tarkastellaan kunnallisten toimintojen muuttamista osakeyhtiömuotoon eli yhtiöittämistä henkilöstön työtyytyväisyyden näkökulmasta. Kyseessä on tapaustutkimus, jossa ilmiötä kuvataan tyypillisten tapausten avulla. Tarkastelun kohteena on neljä Lappeenranta-konserniin kuuluvaa osakeyhtiötä, joiden omistaja on Lappeenrannan kaupunki. Tutkimuksen aineisto kerättiin puolistrukturoiduilla teemahaastatteluilla. Tutkimus on tehty Lappeenrannan kaupungin tarkastuslautakunnan toimeksiannosta. Tutkimustulokset osoittavat, että työtyytymättömyyttä aiheuttavat liiallinen työn määrä, johtaminen, tiukka omistajaohjaus, riittämätön tiedottaminen sekä useat peräkkäiset muutokset. Työtyytyväisyyden pääasiallinen tuottaja on haasteelliset ja mielekkäät työtehtävät, jotka tarjoavat onnistumisen mahdollisuuksia sekä hyvä yhteishenki työpaikalla. Myös yksilön omalla asennoitumisella muutoksiin on ratkaiseva merkitys muutoksista selviytymisessä ja siten työtyytyväisyydessä.

Comparação entre a concentração sérica de alfa-tocoferol de puérperas assistidas em maternidades públicas e privadas no Nordeste do Brasil

OBJETIVO: Comparar a concentração de alfa-tocoferol no soro entre puérperas atendidas em maternidades das redes pública e privada da cidade de Natal (RN), Brasil.MÉTODOS: Participaram do estudo 209 puérperas, sendo 96 mulheres provenientes da rede privada e 113, da rede pública, entre 24 e 48 horas pós-parto. Foram incluídas no estudo parturientes com idade a partir de 12 anos, sem patologias associadas à gestação, que tiveram concepto único sem má-formação. Mulheres descompensadas clinicamente e com gestação múltipla foram excluídas. Amostras de 5 mL de sangue de cada participante foram coletadas no período de jejum, antes da primeira refeição do dia. A concentração de alfa-tocoferol no soro (µg/dL) foi determinada por cromatografia líquida de alta eficiência (CLAE). A diferença estatística entre as médias foi testada utilizando o teste t de Student.RESULTADOS: As médias da concentração de alfa-tocoferol nas puérperas da rede pública e da rede privada, respectivamente, foram 1.115,7±341,4 μg/dL e 1.355,7±397,6 μg/dL, tendo sido observada diferença estatisticamente significante (p=0,000687). Para avaliação individual da concentração de vitamina E, a deficiência foi identificada quando alfa-tocoferol <11,6 μmol/L ou <499,6 µg/dL. As puérperas da rede pública tiveram um percentual de 5,3% (n=6) de deficiência, enquanto nas participantes da rede privada tal carência não foi encontrada. Todavia, baixas concentrações (alfa-tocoferol entre 11,6-16,2 μmol/L ou 499,6-697,7 µg/dL) ocorreram tanto na rede pública como na privada: 9,7% (n=11) e 4,2% (n=4), respectivamente.CONCLUSÃO: Esses resultados destacam que as mulheres assistidas no setor público foram mais vulneráveis a desenvolver baixas concentrações de alfa-tocoferol do que as mulheres assistidas no setor privado.

Puolueiden keskustelutilaisuuksista mediatapahtumiksi. Television vaaliohjelmat ja niihin liittynyt sanomalehtijulkisuus 1960-luvulta 1980-luvulle

Tässä tutkimuksessa tarkastellaan television vaaliohjelmia ja niihin liittynyttä sanomalehtijulkisuutta 1960-luvun alusta 1980-luvun lopulle. Tarkastelun kohteena ovat sekä eduskunta- että presidentinvaalien vaaliohjelmat. Tutkimusaineisto koostuu Yleisradion hallinto- ja ohjelmaneuvostojen pöytäkirjoista, vaaliohjelmien televisiotallenteista sekä vaaliohjelmia käsittelevistä sanomalehtikirjoituksista. Lehtiaineisto on kerätty Helsingin Sanomista, Ilta-Sanomista, Iltalehdestä, Aamulehdestä, Kansan Uutisista, Suomenmaasta sekä Suomen Sosialidemokraatista. Sanomalehtiaineistoa on täydennetty Yleisradion leikearkistoon kerätyillä lehtileikkeillä. Tutkimuksessa on analysoitu toisaalta television vaaliohjelmien kehitystä ja toisaalta vaaliohjelmiin liittynyttä sanomalehtikirjoittelua. Television vaaliohjelmien kehityksen osalta tutkimuksessa on kuvattu, millä tavoin vaaliohjelmia on eri aikoina tehty ja millaisia poliittisia kiistoja niiden tekemiseen on liittynyt. Sanomalehtiaineiston analyysissa on tarkasteltu sitä, mihin seikkoihin vaaliohjelmia käsittelevissä kirjoituksissa on kiinnitetty huomiota, millä tavoin lehdet ovat suhtautuneet ohjelmien toteutukseen ja millainen rooli ohjelmilla on nähty olleen vaalikampanjoinnissa. Väitöskirjan näkökulma on historiallinen, mikä merkitsee ajallisten kontekstien keskeisyyttä analyysissa. Tutkimuksessa on kiinnitetty huomiota sekä poliittisessa kulttuurissa että mediamaisemassa tapahtuneisiin muutoksiin. Vaaliohjelmat olivat 1960-luvulla tarkkaan säänneltyjä puolueiden välisiä keskustelutilaisuuksia, joissa toimittajilla ei ollut näkyvää roolia. Ohjelmien toteutuksesta vastasivat puoluemandaateilla toimineet Yleisradion ohjelma- ja hallintoneuvoston jäsenet, joten ohjelmien toteutuksen yksityiskohdista vastasivat puolueet. Puolueet riitelivät usein vaaliohjelmien toteutuksesta, mikä osoittaa, että puolueille television vaaliohjelmat olivat tärkeitä poliittisia foorumeita jo 1960-luvulta lähtien. Vaaliohjelmat jakautuivat kahteen erilaiseen ohjelmaformaattiin; vaalitentteihin ja suureen vaalikeskusteluun. Vaalitenteissä kunkin puolueen edustajat olivat vuorollaan ”altavastaajina”, joille muiden puolueiden edustajat esittivät kysymyksiä. Suuri vaalikeskustelu oli perinteisempi paneelikeskustelu, jossa poliitikot selvittivät vuorotellen kantojaan ajankohtaisiin poliittisin kysymyksiin. 1970-luvun puolivälissä vaalitenttien toteutuksessa tapahtui suuria muutoksia, kun toimittajat syrjäyttivät poliitikot vaalitenttien kyselijöinä. Suuri vaalikeskustelu säilyi ennallaan. Sanomalehtien suhtautuminen vaaliohjelmiin oli 1960- ja 1970-luvuilla huomattavasti pidättyvämpää kuin poliitikkojen. Sanomalehdistön näkökulmasta television vaaliohjelmien tärkeimpänä tehtävänä oli puolueiden poliittisten linjausten esittely. Vaaliohjelmia käsittelevissä teksteissä esiteltiin pääasiassa poliitikkojen ohjelmissa pitämiä puheenvuoroja. Puoluelehdissä puheenvuorojen sisältöä arvioitiin aatteellisista lähtökohdista, sitoutumattomissa sanomalehdissä neutraalimmin. Vaaliohjelmien toteutukseen liittynyt kritiikki kohdistui toisaalta poliitikkojen puoluepropagandaan, toisaalta poliitikkojen liialliseen varovaisuuteen. Sanomalehtien suhtautuminen vaaliohjelmiin säilyi ennallaan myös 1970-luvulla, jolloin vaaliohjelmia alettiin tehdä toimittajavetoisesti. Ainoa muutos liittyi vaaliohjelmakritiikkiin, joka kohdistui nyt poliitikkojen ohella myös toimittajiin, joiden katsottiin olleen ohjelmissa liian hyökkääviä. Suurin muutos vaaliohjelmiin liittyneessä kirjoittelussa tapahtui 1980-luvulla. Vaaliohjelmia käsitteleviä kirjoituksia julkaistiin sanomalehdistössä monikertainen määrä 1970-lukuun verrattuna. Samalla myös vaaliohjelmia käsittelevien kirjoitusten näkökulmat alkoivat muuttua, kun ohjelmin visuaalinen ulottuvuus alkoi olla yhä näkyvämmin esillä sanomalehtiin laadituissa analyyseissa. Lehdet alkoivat teettää säännöllisesti erilaisia tutkimuksia poliitikkojen pärjäämisestä ohjelmissa ja kirjoittaa vaalikeskusteluiden voittajista ja häviäjistä. Lisäksi lehtijutuissa arvioitiin poliitikkojen esiintymistä ja vaaliohjelmista välittyviä vaikutelmia. Vuoden 1982 presidentinvaaleissa uusista näkökulmista kirjoittivat erityisesti iltapäivälehdet, mutta vuosikymmenen jälkipuoliskolla samankaltaisia lähestymistapoja omaksuivat myös Helsingin Sanomat ja Aamulehti. Niiden vaaliohjelmia käsittelevissä uutisissa kiinnitettiin yhä useammin huomiota poliitikkojen esiintymiseen, pukeutumiseen ja tunnetiloihin. Puoluelehtien suhtautuminen vaaliohjelmiin säilyi kuitenkin ennallaan, ja myös vaaliohjelmakritiikki säilyi suurelta osin muuttumattomana. 1980-luvun aikana television vaaliohjelmat muuttuivat lehdistön käsittelyssä puolueiden tavoitteita esittelevistä keskustelutilaisuuksista poliitikkojen ja puolue johtajien henkilökohtaisia ominaisuuksia mittaaviksi esiintymiskokeiksi ja suuriksi mediatapahtumiksi, joiden katsottiin toisinaan jopa ratkaisseen vaalin tuloksen. Nostaessaan television vaaliohjelmat kampanjajournalisminsa ytimeen, sanomalehdet vahvistivat television poliittista roolia.