827 research outputs found
Silver Threads Among The Gold
Title Onlyhttps://scholarsjunction.msstate.edu/cht-sheet-music/11314/thumbnail.jp
Meditation : Not Ashamed of Christ
https://digitalcommons.library.umaine.edu/mmb-ps/2239/thumbnail.jp
Silver Threads Among the Gold
VERSE 1Darling, I am growing old,Silver threads among the gold,Shine upon my brow today;Life is fading fast away;But, my darling, you will beAlways young and fair to me,Yes! my darling, you will beAlways young and fair to me.
CHORUSDarling, I am growing old.Silver threads among the gold,Shine upon my brow today;Life is fading fast away.
VERSE 2When your hair is silver white,And your cheeks no longer bright,With the roses of the May,I will kiss your lips, and sayOh! My darling, mine aloneYou have never older grown,Yes! my darling, mine alone,You have never older grown!
CHORUS
VERSE 3Love can never more grow old,Locks may lose their brown and gold;Cheeks may fade and hollow grow,But the hearts that love will know,Never, never winter’s frost and chill;Summer warmth is in them stillNever winter’s frost and chill,Summer warmth is in them still.
CHORUS
VERSE 4Love is always young and fair,What to us is silver hair;Faded cheeks, or steps grown slow,To the heart that beats below?Since I kissed you mine alone, alone.You have never older grownSince I kissed you mine alone,Your have never older grown.
CHORU
Silvery Stars Are Softly Gleaming : \b Serenade
https://digitalcommons.library.umaine.edu/mmb-vp/2448/thumbnail.jp
Silvery Stars Are Softly Gleaming : \b Serenade
https://digitalcommons.library.umaine.edu/mmb-vp/2448/thumbnail.jp
My Ole Home in Alabama \u27fo\u27 de War / words by H. P. Danks
Cover: drawing of a poor African American dreaming of an earlier, better life; Publisher: G. D. Russell and Co. (Boston)https://egrove.olemiss.edu/sharris_a/1011/thumbnail.jp
Don\u27t Be Angry with Me Darling / music by H. P. Danks; words by W. L. Gardner
https://egrove.olemiss.edu/sharris_a/1010/thumbnail.jp
STIS Echelle Observations of the Seyfert Galaxy NGC 4151: Physical Conditions in the Ultraviolet Absorbers
We have examined the physical conditions in intrinsic UV-absorbing gas in the
Seyfert galaxy NGC 4151, using echelle spectra obtained with the Space
Telescope Imaging Spectrograph (STIS). We confirm the presence of the kinematic
components detected in earlier GHRS observations as well as a new broad
absorption feature at a radial velocity of -1680 km/s. The UV continuum of NGC
4151 decreased by a factor of 4 over the previous two years, and we argue the
changes in the column density of the low ionization absorption lines associated
with the broad component at -490 km/s reflect the decrease in the ionizing
flux. Most of the strong absorption lines (e.g., N V, C IV, Si IV) from this
component are saturated, but show substantial residual flux in their cores,
indicating that the absorber does not fully cover the source of emission. Our
interpretation is that the unocculted light is due to scattering by free
electrons from an extended region, which reflects continuum, emission lines,
and absorption lines. We have been able to constrain the densities for the
kinematic components based on absorption lines from metastable states of C III
and Fe II, and/or the ratios of ground and fine structure lines of O I,C II,
and Si II. We have generated a set of photoionization models which match the
ionic column densities for each component during the present low flux state and
those seen in previous high flux states with the GHRS and STIS, confirming that
the absorbers are photoionized and respond to the changes in the continuum
flux. We have been able to map the relative radial positions of the absorbers,
and find that the gas decreases in density with distance. None of the UV
absorbers is of sufficiently large column density or high enough ionization
state to account for the X-ray absorption.Comment: 46 pages (Latex), 14 figures (postscript), plus a landscape table
(Latex), to appear in the Astrophysical Journa
HST STIS spectroscopy of the triple nucleus of M31: two nested disks in Keplerian rotation around a Supermassive Black Hole
We present HST spectroscopy of the nucleus of M31 obtained with STIS. Spectra
taken around the CaT lines at 8500 see only the red giants in the double
bright- ness peaks P1 and P2. In contrast, spectra taken at 3600-5100 A are
sensitive to the tiny blue nucleus embedded in P2, the lower surface brightness
red nucleus. P2 has a K-type spectrum, but the embedded blue nucleus has an
A-type spectrum with strong Balmer absorption lines. Given the small likelihood
for stellar collisions, a 200 Myr old starburst appears to be the most
plausible origin of the blue nucleus. In stellar population, size, and velocity
dispersion, the blue nucleus is so different from P1 and P2 that we call it P3.
The line-of-sight velocity distributions of the red stars in P1+P2 strengthen
the support for Tremaine s eccentric disk model. The kinematics of P3 is
consistent with a circular stellar disk in Keplerian rotation around a
super-massive black hole with M_bh = 1.4 x 10^8 M_sun. The P3 and the P1+P2
disks rotate in the same sense and are almost coplanar. The observed velocity
dispersion of P3 is due to blurred rotation and has a maximum value of sigma =
1183+-201 km/s. The observed peak rotation velocity of P3 is V = 618+-81 km/s
at radius 0.05" = 0.19 pc corresponding to a circular rotation velocity at this
radius of ~1700 km/s. Any dark star cluster alternative to a black hole must
have a half-mass radius <= 0.03" = 0.11 pc. We show that this excludes clusters
of brown dwarfs or dead stars on astrophysical grounds.Comment: Astrophysical Journal, Sep 20, 2005, 21 pages including 20 figure
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