Cosmic Origins Research Articles

The Hubble PanCET program: long-term chromospheric evolution and flaring activity of the M dwarf host GJ 3470

Neptune-size exoplanets seem particularly sensitive to atmospheric evaporation, making it essential to characterize the stellar high-energy radiation that drives this mechanism. This is particularly important with M dwarfs, which emit a large and variable fraction of their luminosity in the ultraviolet and can display strong flaring behavior. The warm Neptune GJ 3470b, hosted by an M2 dwarf, was found to harbor a giant exosphere of neutral hydrogen thanks to three transits observed with the Hubble Space Telescope Imaging Spectrograph (HST/STIS). Here we report on three additional transit observations from the Panchromatic Comparative Exoplanet Treasury program, obtained with the HST Cosmic Origin Spectrograph. These data confirm the absorption signature from GJ 3470b’s exosphere in the stellar Lyman-α line and demonstrate its stability over time. No planetary signatures are detected in other stellar lines, setting a 3σ limit on GJ 3470b’s far-ultraviolet (FUV) radius at 1.3 times its Roche lobe radius. We detect three flares from GJ 3470. They show different spectral energy distributions but peak consistently in the Si III line, which traces intermediate-temperature layers in the transition region. These layers appear to play a particular role in GJ 3470’s activity as emission lines that form at lower or higher temperatures than Si III evolved differently over the long term. Based on the measured emission lines, we derive synthetic X-ray and extreme-ultraviolet (X+EUV, or XUV) spectra for the six observed quiescent phases, covering one year, as well as for the three flaring episodes. Our results suggest that most of GJ 3470’s quiescent high-energy emission comes from the EUV domain, with flares amplifying the FUV emission more strongly. The neutral hydrogen photoionization lifetimes and mass loss derived for GJ 3470b show little variation over the epochs, in agreement with the stability of the exosphere. Simulations informed by our XUV spectra are required to understand the atmospheric structure and evolution of GJ 3470b and the role played by evaporation in the formation of the hot-Neptune desert.

The Compact UV Size of Green Pea Galaxies As Local Analogs of High-redshift Lyα-Emitters

Abstract We study the dependence of Lyα escape from galaxies on UV continuum size and luminosity using a sample of 40 Green Pea (GP) galaxies, which are the best local analogs of high-redshift Lyα emitters (LAEs). We use the Cosmic Origins Spectrograph near-ultraviolet images from the Hubble Space Telescope to measure the UV size and luminosity with 0.″047 spatial resolution. Like most galaxies the GPs show a log-normal size distribution. They also show a positive correlation between size and UV-continuum luminosity. The slope of the size-continuum luminosity relation for GPs is consistent with those of continuum-selected star-forming galaxies (SFGs) at low and high redshifts. A distinctive feature of GPs is a very compact typical radius of 0.33 kpc with a population spread (1σ) of 0.19 kpc. The peak of the size distribution and the intercept of the size–luminosity relation of GPs are noticeably smaller than those of continuum-selected SFGs at similar redshifts. There are statistically significant anticorrelations found between the circularized half-light radius (r cir,50), the Lyα equivalent width (EW(Lyα)), and the Lyα escape faction ( ), suggesting that small UV-continuum radii are crucial for Lyα emission. GPs and high-redshift LAEs have similar sizes, once spatial resolution effects are properly considered. Our results show that a compact small size is crucial for escape of Lyα photons, and that Lyα emitters show constant characteristic size independent of their redshift.

High Latitude Zones of GeV Heavy Ions at the Inner Edge of Jupiter's Relativistic Electron Belt

AbstractJuno has discovered signatures of a high energy heavy ion population (>100 MeV/nucleon) within the inner edge of Jupiter's relativistic electron belt. The particles were detected in narrow zones in the high‐latitude lobes of the synchrotron emission region, a location never explored by prior spacecraft (∼31°–46° magnetic latitude; radial distances 1.12–1.41 Jovian radii, M‐shells 1.5–2.37). The population was revealed by extremely high signal ionization signatures seen in images collected by Juno's Stellar Reference Unit star camera (equivalent to 0.2–0.7 MeV of deposited energy per pixel). Signature morphology indicates a population of GeV ions (Z > 1) with atomic mass as high as sulfur, although species with 2 ≤ Z ≤ 8 potentially account for all of the signatures. The detections have occurred while the spacecraft is magnetically connected to Jupiter's halo and gossamer rings, but not while it is connected to the main ring; similar to equatorial observations of GeV carbon and sulfur ions by the Galileo Probe. We find that the particles reside on magnetic drift shells that suggest they are stably trapped within Jupiter's magnetosphere. Because the cosmic ray albedo neutron decay mechanism can only produce protons and electrons, it cannot be the source of this trapped Z > 1 ion population; other galactic cosmic ray origins are suspected. Inward radial transport of tens of keV heavy ions from the outer magnetosphere is another potential source.

New Evidence for Extended He ii Reionization at z ≳ 3.5 from He ii Lyman Alpha and Beta Transmission Spikes*

Abstract We present new high-resolution (R = λ/Δλ ∼ 14,000) spectra of the two brightest He ii-transparent quasars in the far-UV at z em > 3.5, HE2QS J2311−1417 (z em = 3.70) and HE2QS J1630+0435 (z em = 3.81), obtained with the Cosmic Origins Spectrograph on the Hubble Space Telescope. In the predominantly saturated He ii absorption spectra, both sight lines show several isolated resolved (FWHM ≳ 50 km s−1) transmission spikes in He ii Lyα and He ii Lyβ. The incidence of such spikes decreases with increasing redshift, but both sight lines show significant spikes at z ≳ 3.5, signaling the presence of fully ionized regions in the z ≳ 3.5 intergalactic medium (IGM). We employ an automated algorithm to compare the number of detected He ii transmission spikes to predictions from mock spectra created from the outputs of a cubic (146 cMpc)3 optically thin Nyx hydrodynamical simulation, assuming a range of UV background photoionization rates ΓHe II . From the incidence of Lyα and Lyβ transmission spikes we infer similar photoionization rates of at 3.51 < z < 3.66 and ΓHe II = (0.9 ± 0.3) × 10−15 s−1 at 3.460 < z < 3.685, respectively. Because the transmission spikes indicate fully ionized regions at z ≳ 3.5 along both lines of sight, our observations provide further evidence that He ii reionization had substantially progressed at these redshifts.

CGM2 I: The Extent of the Circumgalactic Medium Traced by Neutral Hydrogen

Abstract We present initial results from the Cosmic Origins Spectrograph (COS) and Gemini Mapping the Circumgalactic Medium (CGMCGM ≡ CGM2) survey. The CGM2 survey consists of 1689 galaxies, all with high-quality Gemini-GMOS spectra, within 1 Mpc of 22 z ≲ 1 quasars, all with a signal-to-noise ratio of ∼10 Hubble Space Telescope/COS G130M+G160M spectra. For 572 of these galaxies with stellar masses 107 M ⊙ < M ⋆ < 1011 M ⊙ and z ≲ 0.5, we show that the H i covering fraction above a threshold of N HI > 1014cm−2 is ≳0.5 within 1.5 virial radii (R vir ∼ R 200m). We examine the H i kinematics and find that the majority of absorption lies within ±250 km s−1 of the galaxy systemic velocity. We examine H i covering fractions over a range of impact parameters to infer a characteristic size of the CGM, , as a function of galaxy mass. is the impact parameter at which the probability of observing an absorber with N HI >1014 cm−2 is >50%. In this framework, the radial extent of the CGM of M ⋆ > 109.9 M ⊙ galaxies is kpc or . Intermediate-mass galaxies with 109.2 < M ⋆/M ⊙ < 109.9 have an extent of kpc or . Low-mass galaxies, M ⋆ < 109.2 M ⊙, show a smaller physical scale of kpc and extend to . Our analysis suggests that using R vir as a proxy for the characteristic radius of the CGM likely underestimates its extent.

A CO-to-H2 Ratio of ≈10−5 toward the Herbig Ae Star HK Ori

Abstract Measurements of gas mass in protoplanetary gas disks form the basis for estimating the conditions of planet formation. Among the most important constraints derived from disk diagnostics are the abundances of gas-phase species critical for understanding disk chemistry. Toward this end, we present direct line-of-sight measurements of H2 and CO, employing UV absorption spectroscopy from Hubble Space Telescope Cosmic Origins Spectrograph to characterize disk composition, molecular excitation temperatures, and spatial distribution in the circumstellar material around the Herbig Ae stars HK Ori and T Ori. We observe strong CO (N(CO) = 1015.5 cm−2; T rot(CO) = 19 K) and H2 (N(H2) = 1020.34 cm−2; T rot(H2) = 141 K) absorption toward HK Ori with a CO/H2 ratio of (≡N(CO)/N(H2)) = × 10−5. These measurements place direct empirical constraints on the CO-to-H2 conversion factor in the disk around a Herbig Ae star for the first time, although there is uncertainty concerning the exact viewing geometry of the disk. The spectra of T Ori show CO (N(CO) = 1014.9 cm−2; T rot(CO) = 124 K) absorption. Interestingly, we do not detect any H2 absorption toward this star (N(H2) < 1015.9 cm−2). We discuss a potential scenario for the detection of CO without H2, which deserves further investigation. The low abundance ratio measured around HK Ori suggests significant depletion of CO in the circumstellar gas, which conforms with the handful of other recent CO abundance measurements in protoplanetary disks.

Giant Galaxies from the Universe's Childhood Challenge Cosmic Origin Stories

Giant Galaxies from the Universe's Childhood Challenge Cosmic Origin Stories

Lyman continuum leakage from low-mass galaxies with M⋆ < 108 M⊙

ABSTRACT We present observations with the Cosmic Origins Spectrograph onboard the Hubble Space Telescope of nine low-mass star-forming galaxies at redshifts, z, in the range 0.3179–0.4524, with stellar masses $M_\star \, \lt $ 108 M⊙ and very high specific star-formation rates sSFR ∼150–630 Gyr−1, aiming to study the dependence of leaking Lyman continuum (LyC) emission on stellar mass and some other characteristics of the galaxy. We detect LyC emission in four out of nine galaxies with escape fractions, fesc(LyC), in the range of 11–35 per cent, and establish upper limits for fesc(LyC) in the remaining five galaxies. We observe a narrow Ly α emission line with two peaks in seven galaxies and likely more complex Ly α profiles in the two remaining galaxies. The velocity separation between the peaks Vsep varies in the range from ∼229 to ∼512 km s−1. Our additional data on low-mass galaxies confirm and strengthen the tight anticorrelation between fesc(LyC) and Vsep found for previous low-redshift galaxy samples with higher stellar masses. Vsep remains the best indirect indicator of LyC leakage. It is better than O32 on which fesc(LyC) depends weakly, with a large scatter. Finally, contrary to expectations, we find no increase of fesc(LyC) with decreasing galaxy stellar mass M⋆.

In the Trenches of the Solar–Stellar Connection. III. The HST/COS Ecliptic-poles Stellar Survey (EclipSS)

Abstract The Ecliptic-poles Stellar Survey (EclipSS) collected far-ultraviolet (FUV: 1160–1420 Å) spectra of 49 nearby (d ≲ 100 pc) F3–K3 main-sequence stars, located at high ecliptic latitudes (north and south), using the Cosmic Origins Spectrograph of the Hubble Space Telescope. The ecliptic poles receive higher exposures from scanning missions like the Transiting Exoplanet Survey Satellite (high-precision optical photometry) and Extended Roentgen Survey with an Imaging Telescope Array (X-ray monitoring), which can deliver crucial contextual information, not otherwise easily secured. The objective was to support theoretical studies of stellar hot outer atmospheres—chromospheres (∼104 K) and coronae (≳1 MK)—which, among other things, can adversely impact exoplanets via host-star “space weather.” Flux–flux diagrams (e.g., C ii 1335 Å versus O i 1306 Å) were constructed for the EclipSS stars, solar Cycle 23/24 irradiances, and long-term FUV records of α Cen A (G2 V) and B (K1 V). The EclipSS cohort displays similar minimum (“basal”) fluxes to the Sun and solar twin α Cen A, in chromospheric O i 1306 Å. In hotter C ii 1335 Å, a downward slump of the basal fluxes—noted in previous, less controlled surveys—can now be explained as an effect of subsolar abundances. The consistent basal minima in chromospheric and higher temperature species at solar metallicity favor the idea that stellar analogs of the solar supergranulation network provide a baseline of high-energy emissions. The magnetic network is replenished by a “local dynamo” independently of the stellar spin. It can operate even when the starspot-spawning internal dynamo has ceased cycling, as during the Sun’s 17th century Maunder Minimum.

The relation between Lyαabsorbers and local galaxy filaments

Context.The intergalactic medium (IGM) is believed to contain the majority of baryons in the universe and to trace the same dark matter structure as galaxies, forming filaments and sheets. Lyαabsorbers, which sample the neutral component of the IGM, have been extensively studied at low and high redshift, but the exact relation between Lyαabsorption, galaxies, and the large-scale structure is observationally not well constrained.Aims.In this study, we aim at characterising the relation between Lyαabsorbers and nearby over-dense cosmological structures (galaxy filaments) at recession velocities Δv ≤ 6700 km s−1by using archival observational data from various instruments.Methods.We analyse 587 intervening Lyαabsorbers in the spectra of 302 extragalactic background sources obtained with the Cosmic Origins Spectrograph (COS) installed on theHubbleSpace Telescope (HST). We combine the absorption line information with galaxy data of five local galaxy filaments from the V8k catalogue.Results.Along the 91 sightlines that pass close to a filament, we identify 215 (227) Lyαabsorption systems (components). Among these, 74 Lyαsystems are aligned in position and velocity with the galaxy filaments, indicating that these absorbers and the galaxies trace the same large-scale structure. The filament-aligned Lyαabsorbers have a ∼90% higher rate of incidence (d𝒩/dz = 189 for logN(H I) ≥ 13.2) and a slightly shallower column density distribution function slope (−β = −1.47) relative to the general Lyαpopulation atz = 0, reflecting the filaments’ matter over-density. The strongest Lyαabsorbers are preferentially found near galaxies or close to the axis of a filament, although there is substantial scatter in this relation. Our sample of absorbers clusters more strongly around filament axes than a randomly distributed sample would do (as confirmed by a Kolmogorov–Smirnov test), but the clustering signal is less pronounced than for the galaxies in the filaments.

The Wolf–Rayet + Black Hole Binary NGC 300 X-1: What is the Mass of the Black Hole?

Abstract We present new X-ray and UV observations of the Wolf–Rayet + black hole (BH) binary system NGC 300 X-1 with the Chandra X-ray Observatory and the Hubble Space Telescope Cosmic Origins Spectrograph. When combined with archival X-ray observations, our X-ray and UV observations sample the entire binary orbit, providing clues to the system geometry and interaction between the BH accretion disk and the donor star wind. We measure a binary orbital period of 32.7921 ± 0.0003 hr, in agreement with previous studies, and perform phase-resolved spectroscopy using the X-ray data. The X-ray light curve reveals a deep eclipse, consistent with inclination angles of i = 60°–75°, and a pre-eclipse excess consistent with an accretion stream impacting the disk edge. We further measure radial velocity variations for several prominent far-UV spectral lines, most notably H ii λ1640 and C iv λ1550. We find that the He ii emission lines systematically lag the expected Wolf–Rayet star orbital motion by a phase difference of Δϕ ∼ 0.3, while C iv λ1550 matches the phase of the anticipated radial velocity curve of the Wolf–Rayet donor. We assume the C iv λ1550 emission line follows a sinusoidal radial velocity curve (semi-amplitude = 250 km s−1) and infer a BH mass of 17 ± 4 M ⊙. Our observations are consistent with the presence of a wind-Roche lobe overflow accretion disk, where an accretion stream forms from gravitationally focused wind material and impacts the edge of the BH accretion disk.

Spectral Shapes of the Lyα Emission from Galaxies. I. Blueshifted Emission and Intrinsic Invariance with Redshift*

Abstract We demonstrate the redshift evolution of the spectral profile of H i Lyα emission from star-forming galaxies. In this first study we pay special attention to the contribution of blueshifted emission. At redshift z = 2.9–6.6, we compile spectra of a sample of 229 Lyα-selected galaxies identified with the Multi-Unit Spectroscopic Explorer at the Very Large Telescope, while at low z ( < 0.44) we use a sample of 74 ultraviolet-selected galaxies observed with the Cosmic Origin Spectrograph on board the Hubble Space Telescope. At low z, where absorption from the intergalactic medium (IGM) is negligible, we show that the ratio of Lyα luminosity blueward and redward of line center (L B/R) increases rapidly with increasing equivalent width (W Lyα ). This correlation does not, however, emerge at z = 3–4, and we use bootstrap simulations to demonstrate that trends in L B/R should be suppressed by variations in IGM absorption. Our main result is that the observed blueshifted contribution evolves rapidly downward with increasing redshift: L B/R ≈ 30% at z ≈ 0, but dropping to 15% at z ≈ 3, and to below 3% by z ≈ 6. Applying further simulations of the IGM absorption to the unabsorbed COS spectrum, we demonstrate that this decrease in the blue-wing contribution can be entirely attributed to the thickening of intervening Lyα absorbing systems, with no need for additional H i opacity from local structure, companion galaxies, or cosmic infall. We discuss our results in light of the numerical radiative transfer simulations, the evolving total Lyα and ionizing output of galaxies, and the utility of resolved Lyα spectra in the reionization epoch.

FUV Observations of the Inner Coma of 46P/Wirtanen

Abstract Far-ultraviolet observations of comets yield information about the energetic processes that dissociate the sublimated gases from their primitive surfaces. Understanding which emission processes are dominant, their effects on the observed cometary spectrum, and how to properly invert the spectrum back to the composition of the presumably pristine surface ices of a comet nuclei are all critical components for proper interpretation and analysis of comets. The close approach of comet 46P/Wirtanen in 2018–2019 provided a unique opportunity to study the innermost parts of a cometary coma with the Hubble Space Telescope Cosmic Origins Spectrograph, rarely accessible with remote observations, at length scales (hundreds of kilometers) and wavelengths (900–1430 Å) previously probed only by the European Space Agency’s Rosetta spacecraft. Our observations show a complex picture for the inner coma; atomic production rates for H and O that show water is the dominant source of both, an abundance of atomic sulfur that is difficult to explain with the lifetimes of common sulfur parent molecules, and a density distribution that is poorly fit with both Haser and vectorial models.

Tracing gold’s cosmic origin story

Astronomers thought they had finally figured out where the gold, platinum, and other heavy elements in the universe came from. In light of recent results, they’re not so sure. Desperate phone calls made in the dead of night rarely convey good news, much less first word of a major scientific discovery. Alex Ji made such a call in 2015 from atop a mountain in Chile, where he was using one of the world’s largest telescopes. “This was actually the first time that I had taken data on a telescope ever,” says Ji, then a graduate student at the Massachusetts Institute of Technology in Cambridge. “I was absolutely convinced that I had done something wrong.” How does the universe make heavy elements such as gold? It’s a question astronomers have wrestled with for more than half a century—and the answers are only starting to emerge. Image credit: Science Source/Tom McHugh. So, just after midnight, Ji called his advisor Anna Frebel to describe what he had just seen and could barely believe: A faint star in a dim nearby galaxy named Reticulum II seemed to have extraordinary amounts of europium, an element that’s even rarer in the cosmos than gold. Frebel told Ji to observe another star in the same small galaxy. That star also turned out to be rich in europium, as did a third. In the end, seven of the nine stars Ji observed had extreme levels of the rare element. It would take some time for the astronomers to interpret their surprising result, but when they did, it bore on one of the most pressing questions in astronomy: How does the universe make its heaviest elements? It’s a question astronomers have wrestled with for more than half a century. Elements such as gold, silver, and platinum don’t normally form …

NGTS and HST insights into the long-period modulation in GW Librae

ABSTRACT Light curves of the accreting white dwarf pulsator GW Librae spanning a 7.5-month period in 2017 were obtained as part of the Next-Generation Transit Survey. This data set comprises 787 h of photometry from 148 clear nights, allowing the behaviour of the long (hours) and short-period (20 min) modulation signals to be tracked from night to night over a much longer observing baseline than has been previously achieved. The long-period modulations intermittently detected in previous observations of GW Lib are found to be a persistent feature, evolving between states with periods ≃ 83 min and 2–4 h on time-scales of several days. The 20 min signal is found to have a broadly stable amplitude and frequency for the duration of the campaign, but the previously noted phase instability is confirmed. Ultraviolet observations obtained with the Cosmic Origin Spectrograph on-board the Hubble Space Telescope constrain the ultraviolet-to-optical flux ratio to ≃5 for the 4 h modulation, and ≲1 for the 20 min period, with caveats introduced by non-simultaneous observations. These results add further observational evidence that these enigmatic signals must originate from the white dwarf, highlighting our continued gap in theoretical understanding of the mechanisms that drive them.

Solar Cycle, Maunder Minimum and Pandemic Influenza

We explore the idea that influenza pandemics may arise from the transference of new virions (new sub-types of the influenza virus) of cosmic origin in general accord with the theory of cometary panspermia. Such a transfer process will be modulated by the sunspot cycle and through its role in affecting the interplanetary magnetic field configurations in the Earth’s vicinity. Transfers of virus could take place directly from comets or indirectly from a transient repository represented for instance by the Kordylewski if dust clouds at the L4 and L5 Lagrange libration points of the Earth-Moon system. In either case an active sun appears to be a perequisite for effective transfers. The long remission of influenza pandemics throughout the period 1645-1715, during the Maunder sunspot minimum, might be understood on the basis of our model.

Solar Cycle, Maunder Minimum and Pandemic Influenza

We explore the idea that influenza pandemics may arise from the transference of new virions (new sub-types of the influenza virus) of cosmic origin in general accord with the theory of cometary panspermia. Such a transfer process will be modulated by the sunspot cycle and through its role in affecting the interplanetary magnetic field configurations in the Earth’s vicinity. Transfers of virus could take place directly from comets or indirectly from a transient repository represented for instance by the Kordylewski if dust clouds at the L4 and L5 Lagrange libration points of the Earth-Moon system. In either case an active sun appears to be a perequisite for effective transfers. The long remission of influenza pandemics throughout the period 1645-1715, during the Maunder sunspot minimum, might be understood on the basis of our model.

Crimean observations of the magnetic Sun: 1967–2018

The magnetic field measurements of the Sun as a star initiated by academician A.B. Severny have been supported by six other observatories. The history of such investigations at CrAO and the basic results are briefly described. The synodic spin period of the gravitating solar mass P⊙ = 27.027(6) days is determined; the latter is shown to be linked to the Earth’s motion: the Sun makes 27 semi-revolutions over one terrestrial year, and the Earth – the same number of its revolutions with the period PD during one full solar rotation. The field changes with the Hale cycle PH ≈ 22 years and the cycle P7 = 7 years, whereas their ratio coincides with the Archimedes approximation, 22:7, for the π number, the timescale (π - 3)P7 = P⊙2/2PD – with the Earth’s orbital period. We provide arguments in favour of the cosmic origin of both cycles and holographic expressions, including PH, P7, π, and universal constants.

An accurate reconstruction of CMB E-mode signal over large angular scales using prior information of CMB covariance matrix in ILC algorithm

ABSTRACT Recently, the internal-linear-combination (ILC) method was investigated extensively in the context of reconstruction of Cosmic Microwave Background (CMB) temperature anisotropy signal using observations obtained by WMAP and Planck satellite missions. In this article, we, for the first time, apply the ILC method to reconstruct the large-scale CMB E mode polarization signal, which could probe the ionization history, using simulated observations of 15 frequency CMB polarization maps of future generation Cosmic Origin Explorer (COrE) satellite mission. We find that the clean power spectra, from the usual ILC, are strongly biased due to non-zero CMB-foregrounds chance correlations. In order to address the issues of bias and errors we extend and improve the usual ILC method for CMB E-mode reconstruction by incorporating prior information of theoretical E-mode angular power spectrum while estimating the weights for linear combination of input maps (Sudevan & Saha 2018b). Using the E-mode covariance matrix effectively suppresses the CMB-foreground chance correlation power leading to an accurate reconstruction of cleaned CMB E-mode map and its angular power spectrum. We compare the performance of the usual ILC and the new method over large angular scales and show that the later produces significantly statistically improved results than the former. The new E-mode CMB angular power spectrum contains neither any significant negative bias at the low multipoles nor any positive foreground bias at relatively higher mutltipoles. The error estimates of the cleaned spectrum agree very well with the cosmic variance induced error.

Человек во времени: Россия — последнее столетие

The last century is filled with victories and failures, passions, and interests. World wars and revolutions, the change of political regimes, ideologies, and ideological orientations — all this provoked a formation of social and political chaos, which sometimes had to be overcome in a totalitarian way through sole commanding and by one-party dictatorship. At the same time, one can observe the successes of cognition, culture, scientific and technological development, which, however, can hardly be called “progress”. Because the mass destruction weapons of certain “partners” in globalism have also been increased. Ready for self-destruction, “man in time” did not become yet the master of his destiny in the last century, but in many ways remained a mystery to himself. Despite the fact that over the past century man has learned a lot about his own psychology, consciousness and subconscious, he still needs further self-knowledge no less than in those times when the Oracle of Delphi called for it. Today, as ancient times, one needs to know better what motivates his sometimes rational, and sometimes, mildly speaking, very strange behavior. Who is man in time? To understand this, one must go beyond the limits of itself being to other times and spaces. Even to times and spaces of a cosmic scale, to the spaces and to the depths of our Universe, where a man was born and will disappear, perhaps preserved in its cosmic memory. The memory of the Universe is symbolized by world constants that arose as a result of the Big Bang and the birth of the Universe from a singularity point. Memory of man inherits this property of the Cosmos. The memory is a system-forming factor that creates man and its world. This is what rigorous science can offer to explain the cosmic origin of man and his memory. Artistic imagery can continue the efforts of science. Culture, literature, first of all, can create imageries that will tell about man and his time more than abstract theory. The imageries will tell that man has not yet lost his freedom of creativity. He must remember the past, live in the present, look and go to the future.