Silver Threads Among The Gold

Title Onlyhttps://scholarsjunction.msstate.edu/cht-sheet-music/11314/thumbnail.jp

Meditation : Not Ashamed of Christ

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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

My Little Lost Irene

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Silvery Stars Are Softly Gleaming : \b Serenade

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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